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Title: Lectures on Stellar Statistics
Author: Charlier, Carl Vilhelm Ludvig
Language: English
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Copyright Status: Not copyrighted in the United States. If you live elsewhere check the laws of your country before downloading this ebook. See comments about copyright issues at end of book.

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[Transcriber's Note: This text uses utf-8 (unicode) file encoding. If
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α β γ ε λ ο ς ″
make sure your text reader's "character set" or "file encoding" is set
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last resort, use the latin-1 version of the file instead.

In the original text, the units h and m, and ordinals th and st were
printed as superscripts. For readability, they have not been represented
as such in this file. Similarly for the + and - signs when used to
describe intermediate stellar colours.

Other superscripts are indicated by the carat symbol, ^, and subscripts
by an underline, _.]




LUND 1921




1. Our knowledge of the stars is based on their _apparent_ attributes,
obtained from the astronomical observations. The object of astronomy is
to deduce herefrom the real or _absolute_ attributes of the stars, which
are their position in space, their movement, and their physical nature.

The apparent attributes of the stars are studied by the aid of their
_radiation_. The characteristics of this radiation may be described in
different ways, according as the nature of the light is defined.
(Undulatory theory, Emission theory.)

From the statistical point of view it will be convenient to consider the
radiation as consisting of an emanation of small particles from the
radiating body (the star). These particles are characterized by certain
attributes, which may differ in degree from one particle to another.
These attributes may be, for instance, the diameter and form of the
particles, their mode of rotation, &c. By these attributes the optical
and electrical properties of the radiation are to be explained. I shall
not here attempt any such explanation, but shall confine myself to the
property which the particles have of possessing a different mode of
deviating from the rectilinear path as they pass from one medium to
another. This deviation depends in some way on one or more attributes of
the particles. Let us suppose that it depends on a single attribute,
which, with a terminology derived from the undulatory theory of
HUYGHENS, may be called the _wave-length_ (λ) of the particle.

The statistical characteristics of the radiation are then in the first

(1) the total number of particles or the _intensity_ of the radiation;

(2) the _mean wave-length_ (λ_0) of the radiation, also called (or
nearly identical with) the _effective_ wave-length or the colour;

(3) _the dispersion of the wave-length_. This characteristic of the
radiation may be determined from the _spectrum_, which also gives the
variation of the radiation with λ, and hence may also determine the mean
wave-length of the radiation.

Moreover we may find from the radiation of a star its apparent place on
the sky.

The intensity, the mean wave-length, and the dispersion of the
wave-length are in a simple manner connected with the _temperature_
(_T_) of the star. According to the radiation laws of STEPHAN and WIEN
we find, indeed (compare L. M. 41[1]) that the intensity is proportional
to the fourth power of _T_, whereas the mean wave-length and the
dispersion of the wave-length are both inversely proportional to _T_. It
follows that with increasing temperature the mean wave-length
diminishes--the colour changing into violet--and simultaneously the
dispersion of the wave-length and also even the total length of the
spectrum are reduced (decrease).

2. _The apparent position of a star_ is generally denoted by its right
ascension (α) and its declination (δ). Taking into account the apparent
distribution of the stars in space, it is, however, more practical to
characterize the position of a star by its galactic longitude (_l_) and
its galactic latitude (_b_). Before defining these coordinates, which
will be generally used in the following pages, it should be pointed out
that we shall also generally give the coordinates α and δ of the stars
in a particular manner. We shall therefore use an abridged notation, so
that if for instance α = 17h 44m.7 and δ = +35°.84, we shall write

    (αδ) = (174435).

If δ is negative, for instance δ = -35°.84, we write

    (αδ) = (1744{35}),

so that the last two figures are in italics.

[Transcriber's Note: In this version of the text, the last two figures
are enclosed in braces to represent the italics.]

This notation has been introduced by PICKERING for variable stars and is
used by him everywhere in the Annals of the Harvard Observatory, but it
is also well suited to all stars. This notation gives, simultaneously,
the characteristic _numero_ of the stars. It is true that two or more
stars may in this manner obtain the same characteristic _numero_. They
are, however, easily distinguishable from each other through other

The _galactic_ coordinates _l_ and _b_ are referred to the Milky Way
(the Galaxy) as plane of reference. The pole of the Milky Way has
according to HOUZEAU and GOULD the position (αδ) = (124527). From the
distribution of the stars of the spectral type B I have in L. M. II,
14[2] found a somewhat different position. But having ascertained later
that the real position of the galactic plane requires a greater number
of stars for an accurate determination of its value, I have preferred to
employ the position used by PICKERING in the Harvard catalogues, namely
(αδ) = (124028), or

    α = 12h 40m = 190°, δ = +28°,

which position is now exclusively used in the stellar statistical
investigations at the Observatory of Lund and is also used in these

The galactic longitude (_l_) is reckoned from the ascending node of the
Milky Way on the equator, which is situated in the constellation
_Aquila_. The galactic latitude (_b_) gives the angular distance of the
star from the Galaxy. On plate I, at the end of these lectures, will be
found a fairly detailed diagram from which the conversion of α and δ of
a star into _l_ and _b_ may be easily performed. All stars having an
apparent magnitude brighter than 4m are directly drawn.

Instead of giving the galactic longitude and latitude of a star we may
content ourselves with giving the galactic _square_ in which the star is
situated. For this purpose we assume the sky to be divided into 48
squares, all having the same surface. Two of these squares lie at the
northern pole of the Galaxy and are designated GA_1 and GA_2. Twelve lie
north of the galactic plane, between 0° and 30° galactic latitude, and
are designated GC_1, GC_2, ..., GC_12. The corresponding squares south
of the galactic equator (the plane of the Galaxy) are called GD_1, GD_2,
..., GD_12. The two polar squares at the south pole are called GF_1 and
GF_2. Finally we have 10 B-squares, between the A- and C-squares and 10
corresponding E-squares in the southern hemisphere.

The distribution of the squares in the heavens is here graphically
represented in the projection of FLAMSTEED, which has the advantage of
giving areas proportional to the corresponding spherical areas, an
arrangement necessary, or at least highly desirable, for all stellar
statistical researches. It has also the advantage of affording a
continuous representation of the whole sky.

The correspondence between squares and stellar constellations is seen
from plate II. Arranging the constellations according to their galactic
longitude we find north of the galactic equator (in the C-squares) the

    Hercules, Cygnus, Cepheus, Cassiopæa, Auriga, Gemini, Canis Minor,
    Pyxis, Vela, Centaurus, Scorpius, Ophiuchus,

and south of this equator (in the D-squares):--

    Aquila, Cygnus, Lacerta, Andromeda, Perseus, Orion, Canis Major,
    Puppis, Carina, Circinus, Corona australis, Sagittarius,

mentioning only one constellation for each square.

At the north galactic pole (in the two A-squares) we have:--

    Canes Venatici and Coma Berenices,

and at the south galactic pole (in the two F-squares):--

    Cetus and Sculptor.

3. _Changes in the position of a star._ From the positions of a star on
two or more occasions we obtain its apparent motion, also called the
_proper motion_ of the star. We may distinguish between a _secular_ part
of this motion and a _periodical_ part. In both cases the motion may be
either a reflex of the motion of the observer, and is then called
_parallactic_ motion, or it may be caused by a real motion of the star.
From the parallactic motion of the star it is possible to deduce its
distance from the sun, or its parallax. The periodic parallactic proper
motion is caused by the motion of the earth around the sun, and gives
the _annual parallax_ (π). In order to obtain available annual
parallaxes of a star it is usually necessary for the star to be nearer
to us than 5 siriometers, corresponding to a parallax greater than
0″.04. More seldom we may in this manner obtain trustworthy values for a
distance amounting to 10 siriometers (π = 0″.02), or even still greater
values. For such large distances the _secular_ parallax, which is caused
by the progressive motion of the sun in space, may give better results,
especially if the mean distance of a group of stars is simultaneously
determined. Such a value of the secular parallax is also called, by
KAPTEYN, the _systematic_ parallax of the stars.

When we speak of the proper motion of a star, without further
specification, we mean always the secular proper motion.

4. Terrestrial distances are now, at least in scientific researches,
universally expressed in kilometres. A kilometre is, however, an
inappropriate unit for celestial distances. When dealing with distances
in our planetary system, the astronomers, since the time of NEWTON, have
always used the mean distance of the earth from the sun as universal
unit of distance. Regarding the distances in the stellar system the
astronomers have had a varying practice. German astronomers, SEELIGER
and others, have long used a stellar unit of distance corresponding to
an annual parallax of 0″.2, which has been called a “Siriusweite”. To
this name it may be justly objected that it has no international use, a
great desideratum in science. Against the theoretical definition of this
unit it may also be said that a distance is suitably to be defined
through another distance and not through an angle--an angle which
corresponds moreover, in this case, to the _harmonic_ mean distance of
the star and not to its arithmetic mean distance. The same objection may
be made to the unit “parsec.” proposed in 1912 by TURNER.

For my part I have, since 1911, proposed a stellar unit which, both in
name and definition, nearly coincides with the proposition of SEELIGER,
and which will be exclusively used in these lectures. A _siriometer_ is
put equal to 10^6 times the planetary unit of distance, corresponding to
a parallax of 0″.206265 (in practice sufficiently exactly 0″.2).

In popular writings, another unit: a _light-year_, has for a very long
time been employed. The relation between these units is

    1 siriometer = 15.79   light-years,
    1 light-year =  0.0633 siriometers.

5. In regard to _time_ also, the terrestrial units (second, day, year)
are too small for stellar wants. As being consistent with the unit of
distance, I have proposed for the stellar unit of time a _stellar year_
(st.), corresponding to 10^6 years. We thus obtain the same relation
between the stellar and the planetary units of length and time, which
has the advantage that a _velocity_ of a star expressed in siriometers
per stellar year is expressed with the same numerals in planetary units
of length per year.

Spectroscopic determinations of the velocities, through the
DOPPLER-principle, are generally expressed in km. per second. The
relation with the stellar unit is the following:

    1 km./sec. = 0.2111 sir./st.,
               = 0.2111 planetary units per year,
    1 sir./st. = 4.7375 km./sec.

Thus the velocity of the sun is 20 km./sec. or 4.22 sir./st. (= 4.22
earth distances from the sun per year).

Of the numerical value of the stellar velocity we shall have opportunity
to speak in the following. For the present it may suffice to mention
that most stars have a velocity of the same degree as that of the sun
(in the mean somewhat greater), and that the highest observed velocity
of a star amounts to 72 sir./st. (= 340 km./sec.). In the next chapter I
give a table containing the most speedy stars. The least value of the
stellar velocity is evidently equal to zero.

6. _Intensity of the radiation._ This varies within wide limits. The
faintest star which can give an impression on the photographic plates of
the greatest instrument of the Mount Wilson observatory (100 inch
reflector) is nearly 100 million times fainter than Sirius, a star which
is itself more than 10000 million times fainter than the sun--speaking
of apparent radiation.

The intensity is expressed in _magnitudes_ (_m_). The reason is partly
that we should otherwise necessarily have to deal with very large
numbers, if they were to be proportional to the intensity, and partly
that it is proved that the human eye apprehends quantities of light as
proportional to _m_.

This depends upon a general law in psycho-physics, known as FECHNER's
_law_, which says that changes of the apparent impression of light are
proportional not to the changes of the intensity but to these changes
divided by the primitive intensity. A similar law is valid for all
sensations. A conversation is inaudible in the vicinity of a waterfall.
An increase of a load in the hand from nine to ten hectograms makes no
great difference in the feeling, whereas an increase from one to two
hectograms is easily appreciable. A match lighted in the day-time makes
no increase in the illumination, and so on.

A mathematical analysis shows that from the law of FECHNER it follows
that the impression increases in _arithmetical_ progression (1, 2, 3, 4,
...) simultaneously with an increase of the intensity in _geometrical_
progression (_I_, _I_^2, _I_^3, _I_^4, ...). It is with the sight the
same as with the hearing. It is well known that the numbers of
vibrations of the notes of a harmonic scale follow each other in a
geometrical progression though, for the ear, the intervals between the
notes are apprehended as equal. The magnitudes play the same rôle in
relation to the quantities of light as do the logarithms to the
corresponding numbers. If a star is considered to have a brightness
intermediate between two other stars it is not the _difference_ but the
_ratio_ of the quantities of light that is equal in each case.

The branch of astronomy (or physics) which deals with intensities of
radiation is called _photometry_. In order to determine a certain scale
for the magnitudes we must choose, in a certain manner, the _zero-point_
of the scale and the _scale-ratio_.

Both may be chosen arbitrarily. The _zero-point_ is now almost
unanimously chosen by astronomers in accordance with that used by the
Harvard Observatory. No rigorous definition of the Harvard zero-point,
as far as I can see, has yet been given (compare however H. A. 50[3]),
but considering that the Pole-star (α Ursæ Minoris) is used at Harvard
as a fundamental star of comparison for the brighter stars, and that,
according to the observations at Harvard and those of HERTZSPRUNG (A. N.
4518 [1911]), the light of the Pole-star is very nearly invariable, we
may say that _the zero-point of the photometric scale is chosen in such
a manner that for the Pole-star _m_ = 2.12_. If the magnitudes are given
in another scale than the Harvard-scale (H. S.), it is necessary to
apply the zero-point correction. This amounts, for the Potsdam
catalogue, to -0m.16.

It is further necessary to determine the _scale-ratio_. Our magnitudes
for the stars emanate from PTOLEMY. It was found that the
scale-ratio--giving the ratio of the light-intensities of two
consecutive classes of magnitudes--according to the older values of the
magnitudes, was approximately equal to 2½. When exact photometry began
(with instruments for measuring the magnitudes) in the middle of last
century, the scale-ratio was therefore put equal to 2.5. Later it was
found more convenient to choose it equal to 2.512, the logarithm of
which number has the value 0.4. The magnitudes being themselves
logarithms of a kind, it is evidently more convenient to use a simple
value of the logarithm of the ratio of intensity than to use this ratio
itself. This scale-ratio is often called the POGSON-scale (used by
POGSON in his “Catalogue of 53 known variable stars”, Astr. Obs. of the
Radcliffe Observatory, 1856), and is now exclusively used.

It follows from the definition of the scale-ratio that two stars for
which the light intensities are in the ratio 100:1 differ by exactly 5
magnitudes. A star of the 6th magnitude is 100 times fainter than a star
of the first magnitude, a star of the 11th magnitude 10000 times, of the
16th magnitude a million times, and a star of the 21st magnitude 100
million times fainter than a star of the first magnitude. The star
magnitudes are now, with a certain reservation for systematic errors,
determined with an accuracy of 0m.1, and closer. Evidently, however,
there will correspond to an error of 0.1 in the magnitude a considerable
uncertainty in the light ratios, when these differ considerably from
each other.

    Sun         -26m.60
    Full moon   -11m.77
    Venus       - 4m.28
    Jupiter     - 2m.35
    Mars        - 1m.79
    Mercury     - 0m.90
    Saturn      + 0m.88
    Uranus      + 5m.86
    Neptune     + 7m.66

A consequence of the definition of _m_ is that we also have to do with
_negative_ magnitudes (as well as with negative logarithms). Thus, for
example, for _Sirius_ _m_ = -1.58. The magnitudes of the greater
planets, as well as those of the moon and the sun, are also negative, as
will be seen from the adjoining table, where the values are taken from
“Die Photometrie der Gestirne” by G. MÜLLER.

The apparent magnitude of the sun is given by ZÖLLNER (1864). The other
values are all found in Potsdam, and allude generally to the maximum
value of the apparent magnitude of the moon and the planets.

The brightest star is _Sirius_, which has the magnitude _m_ = -1.58. The
magnitude of the faintest visible star evidently depends on the
penetrating power of the instrument used. The telescope of WILLIAM
HERSCHEL, used by him and his son in their star-gauges and other stellar
researches, allowed of the discerning of stars down to the 14th
magnitude. The large instruments of our time hardly reach much farther,
for visual observations. When, however, photographic plates are used, it
is easily possible to get impressions of fainter stars, even with rather
modest instruments. The large 100-inch mirror of the Wilson Observatory
renders possible the photographic observations of stars of the 20th
apparent magnitude, and even fainter.

The observations of visual magnitudes are performed almost exclusively
with the photometer of ZÖLLNER in a more or less improved form.

7. _Absolute magnitude._ The apparent magnitude of a star is changed as
the star changes its distance from the observer, the intensity
increasing indirectly as the square of the distance of the star. In
order to make the magnitudes of the stars comparable with each other it
is convenient to reduce them to their value at a certain unit of
distance. As such we choose one siriometer. The corresponding magnitude
will be called the _absolute_ magnitude and is denoted by _M_.[4] We
easily find from the table given in the preceding paragraph that the
absolute magnitude of the sun, according to ZÖLLNER's value of _m_,
amounts to +3.4, of the moon to +31.2. For Jupiter we find _M_ = +24.6,
for Venus _M_ = +25.3. The other planets have approximately _M_ = +30.

For the absolute magnitudes of those stars for which it has hitherto
been possible to carry out a determination, we find a value of _M_
between -8 and +13. We shall give in the third chapter short tables of
the absolutely brightest and faintest stars now known.

8. _Photographic magnitudes._ The magnitudes which have been mentioned
in the preceding paragraphs all refer to observations taken with the
eye, and are called _visual_ magnitudes. The total intensity of a star
is, however, essentially dependent on the instrument used in measuring
the intensity. Besides the eye, the astronomers use a photographic
plate, bolometer, a photo-electric cell, and other instruments. The
difference in the results obtained with these instruments is due to the
circumstance that different parts of the radiation are taken into

The usual photographic plates, which have their principal sensibility in
the violet parts of the spectrum, give us the _photographic_ magnitudes
of the stars. It is, however, to be remarked that these magnitudes may
vary from one plate to another, according to the distributive function
of the plate (compare L. M. 67). This variation, which has not yet been
sufficiently studied, seems however to be rather inconsiderable, and
must be neglected in the following.

The photographic magnitude of a star will in these lectures be denoted
by _m′_, corresponding to a visual magnitude _m_.

In practical astronomy use is also made of plates which, as the result
of a certain preparation (in colour baths or in other ways), have
acquired a distributive function nearly corresponding to that of the
eye, and especially have a maximum point at the same wave-lengths. Such
magnitudes are called _photo-visual_ (compare the memoir of PARKHURST in
A. J. 36 [1912]).

The photographic magnitude of a star is generally determined from
measurements of the diameter of the star on the plate. A simple
mathematical relation then permits us to determine _m′_. The diameter of
a star image increases with the time of exposure. This increase is due
in part to the diffraction of the telescope, to imperfect achromatism or
spherical aberration of the objective, to irregular grinding of the
glass, and especially to variations in the refraction of the air, which
produce an oscillation of the image around a mean position.

The _zero-point_ of the photographic magnitudes is so determined that
this magnitude coincides with the visual magnitude for such stars as
belong to the spectral type A0 and have _m_ = 6.0, according to the
proposal of the international solar conference at Bonn, 1911.

Determinations of the photographic or photo-visual magnitudes may now be
carried out with great accuracy. The methods for this are many and are
well summarised in the Report of the Council of the R. A. S. of the year
1913. The most effective and far-reaching method seems to be that
proposed by SCHWARZSCHILD, called the half-grating method, by which two
exposures are taken of the same part of the sky, while at one of the
exposures a certain grating is used that reduces the magnitudes by a
constant degree.

9. _Colour of the stars._ The radiation of a star is different for
different wave-lengths (λ). As regarding other mass phenomena we may
therefore mention:--(1) the _total radiation_ or intensity (_I_), (2)
the _mean wave-length_ (λ_0), (3) the _dispersion of the wave-length_
(σ). In the preceding paragraphs we have treated of the total radiation
of the stars as this is expressed through their magnitudes. The mean
wave-length is pretty closely defined by the _colour_, whereas the
dispersion of the wave-length is found from the _spectrum_ of the stars.

There are blue (B), white (W), yellow (Y) and red (R) stars, and
intermediate colours. The exact method is to define the colour through
the mean wave-length (and not conversely) or the _effective_ wave-length
as it is most usually called, or from the _colour-index_. We shall
revert later to this question. There are, however, a great many direct
eye-estimates of the colour of the stars.

_Colour corresponding to a given spectrum._

    _Sp._    _Colour_       _Number_
     B3        YW-            161
     A0        YW-            788
     A5        YW             115
     F5        YW, WY-        295
     G5        WY             216
     K5        WY+, Y-        552
     M         Y, Y+           95
                     Sum ... 2222

_Spectrum corresponding to a given colour._

    _Colour_       _Sp._       _Number_
     W, W+          A0           281
     YW-            A0           356
     YW             A5           482
     YW+, YW-       F3           211
     WY             G4           264
     WY+, Y-        K1           289
     Y, Y+          K4           254
     RY-, RY        K5            85
                        Sum ... 2222

The signs + and - indicate intermediate shades of colour.

The preceding table drawn up by Dr. MALMQUIST from the colour
observations of MÜLLER and KEMPF in Potsdam, shows the connection
between the colours of the stars and their spectra.

The Potsdam observations contain all stars north of the celestial
equator having an apparent magnitude brighter than 7m.5.

We find from these tables that there is a well-pronounced _regression_
in the correlation between the spectra and the colours of the stars.
Taking together all white stars we find the corresponding mean spectral
type to be A0, but to A0 corresponds, upon an average, the colour
yellow-white. The yellow stars belong in the mean to the K-type, but the
K-stars have upon an average a shade of white in the yellow colour. The
coefficient of correlation (_r_) is not easy to compute in this case,
because one of the attributes, the colour, is not strictly graduated
(_i.e._ it is not expressed in numbers defining the colour).[5] Using
the coefficient of contingency of PEARSON, it is, however, possible to
find a fairly reliable value of the coefficient of correlation, and
MALMQUIST has in this way found _r_ = +0.85, a rather high value.

In order to facilitate the discussion of the relation between colour and
spectrum it is convenient to deal here with the question of the spectra
of the stars.

10. _Spectra of the stars._ In order to introduce the discussion I first
give a list of the wave-lengths of the FRAUENHOFER lines in the
spectrum, and the corresponding chemical elements.

    _FRAUENHOFER line_    _Element_          λ
       A                                   759.4
       B                                   686.8
       C(α)               H (hydrogen)     656.3
       D_1                Na (sodium)      589.6
       D_3                He               587.6
       E                  Fe (iron)        527.0
       F(β)               H                486.2
        (γ)               H                434.1
       G                  Ca (calcium)     430.8
       h(δ)               H                410.2
       H(ε)               Ca(H)            396.9
       K                  Ca               393.4

The first column gives the FRAUENHOFER denomination of each line.
Moreover the hydrogen lines α, β, γ, δ, ε are denoted. The second column
gives the name of the corresponding element, to which each line is to be
attributed. The third column gives the wave-length expressed in
millionths of a millimeter as unit (μμ).

On plate III, where the classification of the stellar spectra according
to the Harvard system is reproduced, will be found also the wave-lengths
of the principal H and He lines.

By the visual spectrum is usually understood the part of the radiation
between the FRAUENHOFER lines A to H (λ = 760 to 400 μμ), whereas the
photographic spectrum generally lies between F and K (λ = 500 to 400

In the earliest days of spectroscopy the spectra of the stars were
classified according to their visual spectra. This classification was
introduced by SECCHI and was later more precisely defined by VOGEL. The
three classes I, II, III of VOGEL correspond approximately to the colour
classification into white, yellow, and red stars. Photography has now
almost entirely taken the place of visual observations of spectra, so
that SECCHI's and VOGEL's definitions of the stellar spectra are no
longer applicable. The terminology now used was introduced by PICKERING
and Miss CANNON and embraces a great many types, of which we here
describe the principal forms as they are defined in Part. II of Vol.
XXVIII of the Annals of the Harvard Observatory. It may be remarked that
PICKERING first arranged the types in alphabetical order A, B, C, &c.,
supposing that order to correspond to the temperature of the stars.
Later this was found to be partly wrong, and in particular it was found
that the B-stars may be hotter than those of type A. The following is
the temperature-order of the spectra according to the opinion of the
Harvard astronomers.

_Type O_ (WOLF-RAYET stars). The spectra of these stars consist mainly
of bright lines. They are characterized by the bright bands at
wave-lengths 463 μμ and 469 μμ, and the line at 501 μμ characteristic of
gaseous nebulae is sometimes present.

This type embraces mainly stars of relatively small apparent brightness.
The brightest is γ Velorum with _m_ = 2.22. We shall find that the
absolute magnitude of these stars nearly coincides with that of the
stars of type B.

The type is grouped into five subdivisions represented by the letters
Oa, Ob, Oc, Od and Oe. These subdivisions are conditioned by the varying
intensities of the bright bands named above. The due sequence of these
sub-types is for the present an open question.

Among interesting stars of this type is ζ Puppis (Od), in the spectrum
of which PICKERING discovered a previously unknown series of helium
lines. They were at first attributed (by RYDBERG) to hydrogen and were
called “additional lines of hydrogen”.

_Type B_ (Orion type, Helium stars). All lines are here dark. Besides
the hydrogen series we here find the He-lines (396, 403, 412, 414, 447,
471, 493 μμ).

To this type belong all the bright stars (β, γ, δ, ε, ζ, η and others)
in Orion with the exception of Betelgeuze. Further, Spica and many other
bright stars.

On plate III ε Orionis is taken as representative of this type.

_Type A_ (Sirius type) is characterized by the great intensity of the
hydrogen lines (compare plate III). The helium lines have vanished.
Other lines visible but faintly.

The greater part of the stars visible to the naked eye are found here.
There are 1251 stars brighter than the 6th magnitude which belong to
this type. Sirius, Vega, Castor, Altair, Deneb and others are all

_Type F_ (Calcium type). The hydrogen lines still rather prominent but
not so broad as in the preceding type. The two calcium lines H and K
(396.9, 393.4 μμ) strongly pronounced.

Among the stars of this type are found a great many bright stars
(compare the third chapter), such as Polaris, Canopus, Procyon.

_Type G_ (Sun type). Numerous metallic lines together with relatively
faint hydrogen lines.

To this class belong the sun, Capella, α Centauri and other bright

_Type K._ The hydrogen lines still fainter. The K-line attains its
maximum intensity (is not especially pronounced in the figure of plate

This is, next to the A-type, the most numerous type (1142 stars) among
the bright stars.

We find here γ Andromedæ, β Aquilæ, Arcturus, α Cassiopeiæ, Pollux and
Aldebaran, which last forms a transition to the next type.

_Type M._ The spectrum is banded and belongs to SECCHI's third type. The
flutings are due to titanium oxide.

Only 190 of the stars visible to the naked eye belong to this type.
Generally they are rather faint, but we here find Betelgeuze, α
Herculis, β Pegasi, α Scorpii (Antares) and most variables of long
period, which form a special sub-type _Md_, characterized by bright
hydrogen lines together with the flutings.

Type M has two other sub-types Ma and Mb.

_Type N_ (SECCHI's fourth type). Banded spectra. The flutings are due to
compounds of carbon.

Here are found only faint stars. The total number is 241. All are red.
27 stars having this spectrum are variables of long period of the same
type as Md.

The spectral types may be summed up in the following way:--

    White stars:--SECCHI's type I:--Harvard B and A,
    Yellow  "  :--   "      "  II:--   "    F, G and K,
    Red     "  :--   "      " III:--   "    M,
     "      "  :--   "      "  IV:--   "    N.

The Harvard astronomers do not confine themselves to the types mentioned
above, but fill up the intervals between the types with sub-types which
are designated by the name of the type followed by a numeral 0, 1, 2,
..., 9. Thus the sub-types between A and F have the designations A0, A1,
A2, ..., A9, F0, &c. Exceptions are made as already indicated, for the
extreme types O and M.

11. _Spectral index._ It may be gathered from the above description that
the definition of the types implies many vague moments. Especially in
regard to the G-type are very different definitions indeed accepted,
even at Harvard.[6] It is also a defect that the definitions do not
directly give _quantitative_ characteristics of the spectra. None the
less it is possible to substitute for the spectral classes a continuous
scale expressing the spectral character of a star. Such a scale is
indeed implicit in the Harvard classification of the spectra.

Let us use the term _spectral index_ (_s_) to define a number expressing
the spectral character of a star. Then we may conveniently define this
conception in the following way. Let A0 correspond to the spectral index
_s_ = 0.0, F0 to _s_ = +1.0, G0 to _s_ = +2.0, K0 to _s_ = +3.0 M0 to
_s_ = +4.0 and B0 to _s_ = -1.0. Further, let A1, A2, A3, &c., have the
spectral indices +0.1, +0.2, +0.3, &c., and in like manner with the
other intermediate sub-classes. Then it is evident that to all spectral
classes between B0 and M there corresponds a certain spectral index _s_.
The extreme types O and N are not here included. Their spectral indices
may however be determined, as will be seen later.

Though the spectral indices, defined in this manner, are directly known
for every spectral type, it is nevertheless not obvious that the series
of spectral indices corresponds to a continuous series of values of some
attribute of the stars. This may be seen to be possible from a
comparison with another attribute which may be rather markedly
graduated, namely the colour of the stars. We shall discuss this point
in another paragraph. To obtain a well graduated scale of the spectra it
will finally be necessary to change to some extent the definitions of
the spectral types, a change which, however, has not yet been

12. We have found in §9 that the light-radiation of a star is described
by means of the total intensity (_I_), the mean wave-length (λ_0) and
the dispersion of the wave-length (σ_λ). λ_0 and σ_λ may be deduced from
the spectral observations. It must here be observed that the
observations give, not the intensities at different wave-lengths but,
the values of these intensities as they are apprehended by the
instruments employed--the eye or the photographic plate. For the
derivation of the true curve of intensity we must know the distributive
function of the instrument (L. M. 67). As to the eye, we have reason to
believe, from the bolometric observations of LANGLEY (1888), that the
mean wave-length of the visual curve of intensity nearly coincides with
that of the true intensity-curve, a conclusion easily understood from
DARWIN's principles of evolution, which demand that the human eye in the
course of time shall be developed in such a way that the mean
wave-length of the visual intensity curve does coincide with that of the
true curve (λ = 530 μμ), when the greatest visual energy is obtained (L.
M. 67). As to the dispersion, this is always greater in the true
intensity-curve than in the visual curve, for which, according to §10,
it amounts to approximately 60 μμ. We found indeed that the visual
intensity curve is extended, approximately, from 400 μμ to 760 μμ, a
sixth part of which interval, approximately, corresponds to the
dispersion σ of the visual curve.

In the case of the photographic intensity-curve the circumstances are
different. The mean wave-length of the photographic curve is,
approximately, 450 μμ, with a dispersion of 16 μμ, which is considerably
smaller than in the visual curve.

13. Both the visual and the photographic curves of intensity differ
according to the temperature of the radiating body and are therefore
different for stars of different spectral types. Here the mean
wave-length follows the formula of WIEN, which says that this
wave-length varies inversely as the temperature. The total intensity,
according to the law of STEPHAN, varies directly as the fourth power of
the temperature. Even the dispersion is dependent on the variation of
the temperature--directly as the mean wave-length, inversely as the
temperature of the star (L. M. 41)--so that the mean wave-length, as
well as the dispersion of the wave-length, is smaller for the hot stars
O and B than for the cooler ones (K and M types). It is in this manner
possible to determine the temperature of a star from a determination of
its mean wave-length (λ_0) or from the dispersion in λ. Such
determinations (from λ_0) have been made by SCHEINER and WILSING in
Potsdam, by ROSENBERG and others, though these researches still have to
be developed to a greater degree of accuracy.

14. _Effective wave-length._ The mean wave-length of a spectrum, or, as
it is often called by the astronomers, the _effective_ wave-length, is
generally determined in the following way. On account of the refraction
in the air the image of a star is, without the use of a spectroscope,
really a spectrum. After some time of exposure we get a somewhat round
image, the position of which is determined precisely by the mean
wave-length. This method is especially used with a so-called
_objective-grating_, which consists of a series of metallic threads,
stretched parallel to each other at equal intervals. On account of the
diffraction of the light we now get in the focal plane of the objective,
with the use of these gratings, not only a fainter image of the star at
the place where it would have arisen without grating, but also at both
sides of this image secondary images, the distances of which from the
central star are certain theoretically known multiples of the effective
wave-lengths. In this simple manner it is possible to determine the
effective wave-length, and this being a tolerably well-known function of
the spectral-index, the latter can also be found. This method was first
proposed by HERTZSPRUNG and has been extensively used by BERGSTRAND,
LUNDMARK and LINDBLAD at the observatory of Upsala and by others.

15. _Colour-index._ We have already pointed out in §9 that the colour
may be identified with the mean wave-length (λ_0). As further λ_0 is
closely connected with the spectral index (_s_), we may use the spectral
index to represent the colour. Instead of _s_ there may also be used
another expression for the colour, called the colour-index. This
expression was first introduced by SCHWARZSCHILD, and is defined in the
following way.

We have seen that the zero-point of the photographic scale is chosen in
such a manner that the visual magnitude _m_ and the photographic
magnitude _m′_ coincide for stars of spectral index 0.0 (A0). The
photographic magnitudes are then unequivocally determined. It is found
that their values systematically differ from the visual magnitudes, so
that for type B (and O) the photographic magnitudes are smaller than the
visual, and the contrary for the other types. The difference is greatest
for the M-type (still greater for the N-stars, though here for the
present only a few determinations are known), for which stars if amounts
to nearly two magnitudes. So much fainter is a red star on a
photographic plate than when observed with the eye.

_The difference between the photographic and the visual magnitudes is
called the colour-index (_c_)._ The correlation between this index and
the spectral-index is found to be rather high (_r_ = +0.96). In L. M.
II, 19 I have deduced the following tables giving the spectral-type
corresponding to a given colour-index, and inversely.



|   Spectral        |  Colour-index  |
| type  |   index   |                |
|  B0   |   -1.0    |    -0.46       |
|  B5   |   -0.5    |    -0.23       |
|  A0   |    0.0    |     0.00       |
|  A5   |   +0.5    |    +0.23       |
|  F0   |   +1.0    |    +0.46       |
|  F5   |   +1.5    |    +0.69       |
|  G0   |   +2.0    |    +0.92       |
|  G5   |   +2.5    |    +1.15       |
|  K0   |   +3.0    |    +1.38       |
|  K5   |   +3.5    |    +1.61       |
|  M0   |   +4.0    |    +1.84       |



| Colour-index   |      Spectral     |
|                | index   |   type  |
|                |         |         |
|     -0.4       | -0.70   |   B3    |
|     -0.2       | -0.80   |   B7    |
|      0.0       | +0.10   |   A1    |
|     +0.2       | +0.50   |   A5    |
|     +0.4       | +0.90   |   A9    |
|     +0.6       | +1.30   |   F3    |
|     +0.8       | +1.70   |   F7    |
|     +1.0       | +2.10   |   G1    |
|     +1.2       | +2.50   |   G5    |
|     +1.4       | +2.90   |   G9    |
|     +1.6       | +3.30   |   K3    |
|     +1.8       | +3.70   |   K7    |
|     +2.0       | +4.10   |   M1    |

From each catalogue of visual magnitudes of the stars we may obtain
their photographic magnitude through adding the colour-index. This may
be considered as known (taking into account the high coefficient of
correlation between _s_ and _c_) as soon as we know the spectral type of
the star. We may conclude directly that the number of stars having a
photographic magnitude brighter than 6.0 is considerably smaller than
the number of stars visually brighter than this magnitude. There are,
indeed, 4701 stars for which _m_ < 6.0 and 2874 stars having _m′_ < 6.0.

16. _Radial velocity of the stars._ From the values of α and δ at
different times we obtain the components of the proper motions of the
stars perpendicular to the line of sight. The third component (_W_), in
the radial direction, is found by the DOPPLER principle, through
measuring the displacement of the lines in the spectrum, this
displacement being towards the red or the violet according as the star
is receding from or approaching the observer.

The velocity _W_ will be expressed in siriometers per stellar year
(sir./st.) and alternately also in km./sec. The rate of conversion of
these units is given in §5.

17. Summing up the remarks here given on the apparent attributes of the
stars we find them referred to the following principal groups:--

I. _The position of the stars_ is here generally given in galactic
longitude (_l_) and latitude (_b_). Moreover their equatorial
coordinates (α and δ) are given in an abridged notation (αδ), where the
first four numbers give the right ascension in hours and minutes and the
last two numbers give the declination in degrees, the latter being
printed in italics if the declination is negative.

Eventually the position is given in galactic squares, as defined in §2.

II. _The apparent motion of the stars_ will be given in radial
components (_W_) expressed in sir./st. and their motion perpendicular to
the line of sight. These components will be expressed in one component
(_u_0_) parallel to the galactic plane, and one component (_v_0_)
perpendicular to it. If the distance (_r_) is known we are able to
convert these components into components of the linear velocity
perpendicular to the line of sight (_U_ and _V_).

III. _The intensity of the light_ of the stars is expressed in
magnitudes. We may distinguish between the _apparent_ magnitude (_m_)
and the _absolute_ magnitude (_M_), the latter being equal to the value
of the apparent magnitude supposing the star to be situated at a
distance of one siriometer.

The apparent magnitude may be either the _photographic_ magnitude
(_m′_), obtained from a photographic plate, or the _visual_ magnitude
(_m_) obtained with the eye.

The difference between these magnitudes is called the _colour-index_
(_c_ = _m′_-_m_).

IV. _The characteristics of the stellar radiation_ are the mean
wave-length (λ_0) and the dispersion (σ) in the wave-length. _The mean
wave-length_ may be either directly determined (perhaps as _effective_
wave-length) or found from the spectral type (spectral index) or from
the colour-index.

There are in all eight attributes of the stars which may be found from
the observations:--the spherical position of the star (_l_, _b_), its
distance (_r_), proper motion (_u_0_ and _v_0_), radial velocity (_W_),
apparent magnitude (_m_ or _m′_), absolute magnitude (_M_), spectral
type (_Sp_) or spectral index (_s_), and colour-index (_c_). Of these
the colour-index, the spectral type, the absolute magnitude and also (to
a certain degree) the radial velocity may be considered as independent
of the place of the observer and may therefore be considered not as only
apparent but also as _absolute_ attributes of the stars.

Between three of these attributes (_m_, _M_ and _r_) a mathematical
relation exists so that one of them is known as soon as the other two
have been found from observations.


[Footnote 1: Meddelanden från Lunds Observatorium, No. 41.]

[Footnote 2: Meddelanden från Lunds Astronomiska Observatorium, Serie
II, No. 14.]

[Footnote 3: Annals of the Harvard Observatory, vol. 50.]

[Footnote 4: In order to deduce from _M_ the apparent magnitude at a
distance corresponding to a parallax of 1″ we may subtract 3m.48. To
obtain the magnitude corresponding to a parallax of 0″.1 we may add
1.57. The latter distance is chosen by some writers on stellar

[Footnote 5: The best colour-scale of the latter sort seems to be that

[Footnote 6: Compare H. A. 50 and H. A. 56 and the remarks in L. M. II,



18. In this chapter I shall give a short account of the publications in
which the most complete information on the attributes of the stars may
be obtained, with short notices of the contents and genesis of these
publications. It is, however, not my intention to give a history of
these researches. We shall consider more particularly the questions
relating to the position of the stars, their motion, magnitude, and

19. _Place of the stars._ _Durchmusterungs._ The most complete data on
the position of the stars are obtained from the star catalogues known as
“Durchmusterungs”. There are two such catalogues, which together cover
the whole sky, one--visual--performed in Bonn and called the _Bonner
Durchmusterung_ (B. D.), the other--photographic--performed in Cape _The
Cape Photographic Durchmusterung_ (C. P. D.). As the first of these
catalogues has long been--and is to some extent even now--our principal
source for the study of the sky and is moreover the first enterprise of
this kind, I shall give a somewhat detailed account of its origin and
contents, as related by ARGELANDER in the introduction to the B. D.

B. D. was planned and performed by the Swedish-Finn ARGELANDER (born in
Memel 1799). A scholar of BESSEL he was first called as director in Åbo,
then in Hälsingfors, and from there went in 1836 to Bonn, where in the
years 1852 to 1856 he performed this great _Durchmusterung_. As
instrument he used a FRAUENHOFER comet-seeker with an aperture of 76 mm,
a focal length of 650 mm, and 10 times magnifying power. The field of
sight had an extension of 6°.

In the focus of the objective was a semicircular piece of thin glass,
with the edge (= the diameter of the semicircle) parallel to the circle
of declination. This edge was sharply ground, so that it formed a
narrow dark line perceptible at star illumination. Perpendicular to this
diameter (the “hour-line”) were 10 lines, at each side of a middle line,
drawn at a distance of 7′. These lines were drawn with black oil colour
on the glass.

The observations are performed by the observer A and his assistant B. A
is in a dark room, lies on a chair having the eye at the ocular and can
easily look over 2° in declination. The assistant sits in the room
below, separated by a board floor, at the _Thiede_ clock.

From the beginning of the observations the declination circle is fixed
at a certain declination (whole degrees). All stars passing the field at
a distance smaller than one degree from the middle line are observed.
Hence the name “Durchmusterung”. When a star passes the “hour line” the
magnitude is called out by A, and noted by B together with the time of
the clock. Simultaneously the declination is noted by A in the darkness.
On some occasions 30 stars may be observed in a minute.

The first observation was made on Febr. 25, 1852, the last on March 27,
1859. In all there were 625 observation nights with 1841 “zones”. The
total number of stars was 324198.

The catalogue was published by ARGELANDER in three parts in the years
1859, 1861 and 1862[7] and embraces all stars between the pole and 2°
south of the equator brighter than 9m.5, according to the scale of
ARGELANDER (his aim was to register all stars up to the 9th magnitude).
To this scale we return later. The catalogue is arranged in accordance
with the declination-degrees, and for each degree according to the right
ascension. Quotations from B. D. have the form B. D. 23°.174, which
signifies: Zone +23°, star No. 174.

ARGELANDER's work was continued for stars between δ = -2° and δ = -23°
by SCHÖNFELD, according to much the same plan, but with a larger
instrument (aperture 159 mm, focal length 1930 mm, magnifying power 26
times). The observations were made in the years 1876 to 1881 and include
133659 stars.[8]

The positions in B. D. are given in tenths of a second in right
ascension and in tenths of a minute in declination.

20. _The Cape Photographic Durchmusterung_[9] (C. P. D.). This embraces
the whole southern sky from -18° to the south pole. Planned by GILL, the
photographs were taken at the Cape Observatory with a DALLMEYER lens
with 15 cm. aperture and a focal-length of 135 cm. Plates of 30 × 30 cm.
give the coordinates for a surface of 5 × 5 square degrees. The
photographs were taken in the years 1885 to 1890. The measurements of
the plates were made by KAPTEYN in Groningen with a “parallactic”
measuring-apparatus specially constructed for this purpose, which
permits of the direct obtaining of the right ascension and the
declination of the stars. The measurements were made in the years 1886
to 1898. The catalogue was published in three parts in the years 1896 to

The positions have the same accuracy as in B. D. The whole number of
stars is 454875. KAPTEYN considers the catalogue complete to at least
the magnitude 9m.2.

In the two great catalogues B. D. and C. P. D. we have all stars
registered down to the magnitude 9.0 (visually) and a good way below
this limit. Probably as far as to 10m.

A third great Durchmusterung has for some time been in preparation at
Cordoba in Argentina.[10] It continues the southern zones of SCHÖNFELD
and is for the present completed up to 62° southern declination.

All these Durchmusterungs are ultimately based on star catalogues of
smaller extent and of great precision. Of these catalogues we shall not
here speak (Compare, however, §23).

A great “Durchmusterung”, that will include all stars to the 11th
magnitude, has for the last thirty years been in progress at different
observatories proposed by the congress in Paris, 1888. The observations
proceed very irregularly, and there is little prospect of getting the
work finished in an appreciable time.

21. _Star charts._ For the present we possess two great photographic
star charts, embracing the whole heaven:--The _Harvard Map_ (H. M.) and
the _FRANKLIN-ADAMS Charts_ (F. A. C.).

_The Harvard Map_, of which a copy (or more correctly two copies) on
glass has kindly been placed at the disposal of the Lund Observatory by
Mr. PICKERING, embraces all stars down to the 11th magnitude. It
consists of 55 plates, each embracing more than 900 square degrees of
the sky. The photographs were taken with a small lens of only 2.5 cms.
aperture and about 32.5 cms. focal-length. The time of exposure was one
hour. These plates have been counted at the Lund Observatory by Hans
HENIE. We return later to these counts.

The _FRANKLIN-ADAMS Charts_ were made by an amateur astronomer
FRANKLIN-ADAMS, partly at his own observatory (Mervel Hill) in England,
partly in Cape and Johannesburg, Transvaal, in the years 1905-1912. The
photographs were taken with a _Taylor_ lens with 25 cm. aperture and a
focal-length of 114 cm., which gives rather good images on a field of 15
× 15 square degrees.

The whole sky is here reproduced on, in all, 206 plates. Each plate was
exposed for 2 hours and 20 minutes and gives images of the stars down to
the 17th magnitude. The original plates are now at the observatory in
Greenwich. Some copies on paper have been made, of which the Lund
Observatory possesses one. It shows stars down to the 14th-15th
magnitudes and gives a splendid survey of the whole sky more complete,
indeed, than can be obtained, even for the north sky, by direct
observation of the heavens with any telescope at present accessible in

The F. A. C. have been counted by the astronomers of the Lund
Observatory, so that thus a complete count of the number of stars for
the whole heaven down to the 14th magnitude has been obtained. We shall
later have an opportunity of discussing the results of these counts.

A great star map is planned in connection with the Paris catalogue
mentioned in the preceding paragraph. This _Carte du Ciel_ (C. d. C.) is
still unfinished, but there seems to be a possibility that we shall one
day see this work carried to completion. It will embrace stars down to
the 14th magnitude and thus does not reach so far as the F. A. C., but
on the other hand is carried out on a considerably greater scale and
gives better images than F. A. C. and will therefore be of a great value
in the future, especially for the study of the proper motions of the

22. _Distance of the stars._ As the determination, from the annual
parallax, of the distances of the stars is very precarious if the
distance exceeds 5 sir. (π = 0″.04), it is only natural that the
catalogues of star-distances should be but few in number. The most
complete catalogues are those of BIGOURDAN in the Bulletin astronomique
XXVI (1909), of KAPTEYN and WEERSMA in the publications of Groningen Nr.
24 (1910), embracing 365 stars, and of WALKEY in the “Journal of the
British Astronomical Association XXVII” (1917), embracing 625 stars.
Through the spectroscopic method of ADAMS it will be possible to enlarge
this number considerably, so that the distance of all stars, for which
the spectrum is well known, may be determined with fair accuracy. ADAMS
has up to now published 1646 parallax stars.

23. _Proper motions._ An excellent catalogue of the proper motions of
the stars is LEWIS BOSS's “Preliminary General Catalogue of 6188 stars”
(1910) (B. P. C.). It contains the proper motions of all stars down to
the sixth magnitude (with few exceptions) and moreover some fainter
stars. The catalogue is considered by the editor only as a preliminary
to a greater catalogue, which is to embrace some 25000 stars and is now
nearly completed.

24. _Visual magnitudes._ The Harvard observatory has, under the
direction of PICKERING, made its principal aim to study the
magnitudes of the stars, and the history of this observatory is at the
same time the history of the treatment of this problem. PICKERING, in
the genuine American manner, is not satisfied with the three thirds of
the sky visible from the Harvard observatory, but has also founded a
daughter observatory in South America, at Arequipa in Peru. It is
therefore possible for him to publish catalogues embracing the whole
heaven from pole to pole. The last complete catalogue (1908) of the
magnitudes of the stars is found in the “Annals of the Harvard
Observatory T. 50” (H. 50). It contains 9110 stars and can be considered
as complete to the magnitude 6m.5. To this catalogue are generally
referred the magnitudes which have been adopted at the Observatory of
Lund, and which are treated in these lectures.

A very important, and in one respect even still more comprehensive,
catalogue of visual magnitudes is the “Potsdam General Catalogue” (P. G.
C.) by MÜLLER and KEMPF, which was published simultaneously with H. 50.
It contains the magnitude of 14199 stars and embraces all stars on the
northern hemisphere brighter than 7m.5 (according to B. D.). We have
already seen that the zero-point of H. 50 and P. G. C. is somewhat
different and that the magnitudes in P. G. C. must be increased by
-0m.16 if they are to be reduced to the Harvard scale. The difference
between the two catalogues however is due to some extent to the colour
of the stars, as has been shown by Messrs. MÜLLER and KEMPF.

25. _Photographic magnitudes._ Our knowledge of this subject is still
rather incomplete. The most comprehensive catalogue is the
“Actinometrie” by SCHWARZSCHILD (1912), containing the photographic
magnitudes of all stars in B. D. down to the magnitude 7m.5 between the
equator and a declination of +20°. In all, 3522 stars. The photographic
magnitudes are however not reduced for the zero-point (compare §6).

These is also a photometric photographic catalogue of the stars nearest
to the pole in PARKHURST's “Yerkes actinometry” (1912),[11] which
contains all stars in B. D. brighter than 7m.5 between the pole and 73°
northern declination. The total number of stars is 672.

During the last few years the astronomers of Harvard and Mount Wilson
have produced a collection of “standard photographic magnitudes” for
faint stars. These stars, which are called the _polar sequence_,[12] all
lie in the immediate neighbourhood of the pole. The list is extended
down to the 20th magnitude. Moreover similar standard photographic
magnitudes are given in H. A. 71, 85 and 101.

A discussion of the _colour-index_ (_i.e._, the difference between the
photographic and the visual magnitudes) will be found in L. M. II, 19.
When the visual magnitude and the type of spectrum are known, the
photographic magnitude may be obtained, with a generally sufficient
accuracy, by adding the colour-index according to the table 1 in §15

26. _Stellar spectra._ Here too we find the Harvard Observatory to be
the leading one. The same volume of the Annals of the Harvard
Observatory (H. 50) that contains the most complete catalogue of visual
magnitudes, also gives the spectral types for all the stars there
included, _i.e._, for all stars to 6m.5. Miss CANNON, at the Harvard
Observatory, deserves the principal credit for this great work. Not
content with this result she is now publishing a still greater work
embracing more than 200000 stars. The first four volumes of this work
are now published and contain the first twelve hours of right
ascension, so that half the work is now printed.[13]

27. _Radial velocity._ In this matter, again, we find America to be the
leading nation, though, this time, it is not the Harvard or the Mount
Wilson but the Lick Observatory to which we have to give the honour. The
eminent director of this observatory, W. W. CAMPBELL, has in a high
degree developed the accuracy in the determination of radial velocities
and has moreover carried out such determinations in a large scale. The
“Bulletin” No. 229 (1913) of the Lick Observatory contains the radial
velocity of 915 stars. At the observatory of Lund, where as far as
possible card catalogues of the attributes of the stars are collected,
GYLLENBERG has made a catalogue of this kind for the radial velocities.
The total number of stars in this catalogue now amounts to 1640.[14]

28. Finally I shall briefly mention some comprehensive works on more
special questions regarding the stellar system.

On _variable stars_ there is published every year by HARTWIG in the
“Vierteljahrschrift der astronomischen Gesellschaft” a catalogue of all
known variable stars with needful information about their minima &c.
This is the completest and most reliable of such catalogues, and is
always up to date. A complete historical catalogue of the variables is
given in “Geschichte und Literatur des Lichtwechsels der bis Ende 1915
als sicher veränderlich anerkannten Sterne nebst einem Katalog der
Elemente ihres Lichtwechsels” von G. MÜLLER und E. HARTWIG. Leipzig
1918, 1920.

On _nebulae_ we have the excellent catalogues of DREYER, the “New
General Catalogue” (N. G. C.) of 1890 in the “Memoirs of the
Astronomical Society” vol. 49, the “Index catalogues” (I. C.) in the
same memoirs, vols. 51 and 59 (1895 and 1908). These catalogues contain
all together 13226 objects.

Regarding other special attributes I refer in the first place to the
important Annals of the Harvard Observatory. Other references will be
given in the following, as need arises.


[Footnote 7: “Bonner Sternverzeichnis” in den Astronomischen
Beobachtungen auf der Sternwarte zu Bonn, Dritter bis Fünfter Band. Bonn

[Footnote 8: “Bonner Durchmusterung”, Vierte Sektion. Achter Band der
Astronomischen Beobachtungen zu Bonn, 1886.]

[Footnote 9: “The Cape Photographic Durchmusterung” by DAVID GILL and J.
C. KAPTEYN, Annals of the Cape Observatory, vol. III-V (1896-1900).]

[Footnote 10: “Cordoba Durchmusterung” by J. THOME. Results of the
National Argentine Observatory, vol. 16, 17, 18, 21 (1894-1914).]

[Footnote 11: Aph. J., vol. 36.]

[Footnote 12: H. A., vol. 71.]

[Footnote 13: H. A., vol. 91, 92, 93, 94.]

[Footnote 14: A catalogue of radial velocities has this year been
published by J. VOUTE, embracing 2071 stars. “First catalogue of radial
velocities”, by J. VOUTE. Weltevreden, 1920.]



29. The number of cases in which all the eight attributes of the stars
discussed in the first chapter are well known for one star is very
small, and certainly does not exceed one hundred. These cases refer
principally to such stars as are characterized either by great
brilliancy or by a great proper motion. The principal reason why these
stars are better known than others is that they lie rather near our
solar system. Before passing on to consider the stars from more general
statistical points of view, it may therefore be of interest first to
make ourselves familiar with these well-known stars, strongly
emphasizing, however, the exceptional character of these stars, and
carefully avoiding any generalization from the attributes we shall here

30. _The apparently brightest stars._ We begin with these objects so
well known to every lover of the stellar sky. The following table
contains all stars the apparent visual magnitude of which is brighter
than 1m.5.

The first column gives the current number, the second the name, the
third the equatorial designation (αδ). It should be remembered that the
first four figures give the hour and minutes in right ascension, the
last two the declination, italics showing negative declination. The
fourth column gives the galactic square, the fifth and sixth columns the
galactic longitude and latitude. The seventh and eighth columns give the
annual parallax and the corresponding distance expressed in siriometers.
The ninth column gives the proper motion (μ), the tenth the radial
velocity _W_ expressed in sir./st. (To get km./sec. we may multiply by
4.7375). The eleventh column gives the apparent visual magnitude, the
twelfth column the absolute magnitude (_M_), computed from _m_ with the
help of _r_. The 13th column gives the type of spectrum (_Sp_), and the
last column the photographic magnitude (_m′_). The difference between
_m′_ and _m_ gives the colour-index (_c_).



| 1|         2           |    3     |    4   |  5  |   6   |   7   |   8   |
|  |                     |           Position              |   Distance    |
|  | _Name_              |----------+--------+-----+-------+-------+-------+
|  |                     |   (αδ)    | Square | _l_ |  _b_  |   π   |  _r_ |
|  |                     |          |        |     |       |       | sir.  |
| 1|Sirius               |(0640{16})|  GD_7  | 195°| - 8°  |0″.876 |  0.5  |
| 2|Canopus              |(0621{52})|  GD_8  | 229 | -24   | 0.007 | 29.5  |
| 3|Vega                 |(183338)  |  GC_2  |  30 | +17   | 0.094 |  2.2  |
| 4|Capella              |(050945)  |  GC_5  | 131 | + 5   | 0.066 |  3.1  |
| 5|Arcturus             |(141119)  |  GA_2  | 344 | +68   | 0.075 |  2.7  |
| 6|α Centauri           |(1432{60})|  GD_10 | 284 | - 2   | 0.759 |  0.3  |
| 7|Rigel                |(0509{08})|  GD_6  | 176 | -24   | 0.007 | 29.5  |
| 8|Procyon              |(073405)  |  GC_7  | 182 | +14   | 0.324 |  0.6  |
| 9|Achernar             |(0134{57})|  GE_8  | 256 | -59   | 0.051 |  4.0  |
|10|β Centauri           |(1356{59})|  GC_10 | 280 | + 2   | 0.037 |  5.6  |
|11|Altair               |(194508)  |  GD_1  |  15 | -10   | 0.238 |  0.9  |
|12|Betelgeuze           |(054907)  |  GD_6  | 168 | - 8   | 0.030 |  6.9  |
|13|Aldebaran            |(043016)  |  GD_5  | 149 | -19   | 0.078 |  2.8  |
|14|Pollux               |(073928)  |  GC_6  | 160 | +25   | 0.064 |  3.2  |
|15|Spica                |(1319{10})|  GB_8  | 286 | +51   |  ..   |  ..   |
|16|Antares              |(1623{26})|  GC_11 | 320 | +14   | 0.029 |  7.1  |
|17|Fomalhaut            |(2252{30})|  GE_10 | 348 | -66   | 0.138 |  1.5  |
|18|Deneb                |(203844)  |  GC_2  |  51 | + 1   |  ..   |  ..   |
|19|Regulus              |(100312)  |  GB_6  | 196 | +50   | 0.033 |  6.3  |
|20|β Crucis             |(1241{59})|  GC_10 | 270 | + 3   | 0.008 | 25.8  |
|  |                     |          |        |     |       |       | sir.  |
|  |   Mean              |    ..    |   ..   |  .. |  23°.5|0″.134 |  7.3  |

| 1|         2           |   9  |   10   |    11   |    12   | 13 |  14  |
|  |                     |    Motion     |     Magnitude     | Spectrum  |
|  | _Name_              +------+--------+---------+---------+----+------+
|  |                     | μ    |  _W_   |   _m_   |   _M_   |_Sp_| _m′_ |
|  |                     |      |sir./st.|         |         |    | _m′_ |
| 1|Sirius               | 1″.32|  - 1.56| -1m.58  | -0m.3   |A   |-1.58 |
| 2|Canopus              |  0.02|  + 4.39|  -0.86  |   -8.2  |F   |-0.40 |
| 3|Vega                 |  0.35|  - 2.91|   0.14  |   -1.6  |A   | 0.14 |
| 4|Capella              |  0.44|  + 6.38|   0.21  |   -2.8  |G   | 1.13 |
| 5|Arcturus             |  2.28|  - 0.82|   0.24  |   -1.9  |K   | 1.62 |
| 6|α Centauri           |  3.68|  - 4.69|   0.33  |   +3.2  |G   | 1.25 |
| 7|Rigel                |  0.00|  + 4.77|   0.34  |   -7.0  |B8p | 0.25 |
| 8|Procyon              |  1.24|  - 0.74|   0.48  |   +1.5  |F5  | 1.17 |
| 9|Achernar             |  0.09|   ..   |   0.60  |   -2.4  |B5  | 0.87 |
|10|β Centauri           |  0.04|  + 2.53|   0.86  |   -2.9  |B1  | 0.45 |
|11|Altair               |  0.66|  - 6.97|   0.89  |   +1.2  |A5  | 1.12 |
|12|Betelgeuze           |  0.03|  + 4.43|   0.92  |   -3.3  |Ma  | 2.76 |
|13|Aldebaran            |  0.20|  +11.63|   1.06  |   -1.2  |K5  | 2.67 |
|14|Pollux               |  0.07|  + 0.82|   1.21  |   -1.3  |K   | 2.59 |
|15|Spica                |  0.06|  + 0.34|   1.21  |    ..   |B2  | 0.84 |
|16|Antares              |  0.03|  - 0.63|   1.22  |   -3.0  |Map | 3.06 |
|17|Fomalhaut            |  0.37|  + 1.41|   1.29  |   +0.4  |A3  | 1.43 |
|18|Deneb                |  0.00|  - 0.84|   1.33  |    ..   |A2  | 1.42 |
|19|Regulus              |  0.25|   ..   |   1.34  |   -2.7  |B8  | 1.25 |
|20|β Crucis             |  0.06|  + 2.74|   1.50  |   -5.6  |B1  | 1.09 |
|  |                     |      |        |         |         |    | _m′_ |
|  |   Mean              | 0″.56|    3.26| +0m.64  |  -2m.1  |F1  |+1.13 |

The values of (αδ), _m_, _Sp_ are taken from H. 50. The values of _l_,
_b_ are computed from (αδ) with the help of tables in preparation at the
Lund Observatory, or from the original to plate I at the end, allowing
the conversion of the equatorial coordinates into galactic ones. The
values of π are generally taken from the table of KAPTEYN and WEERSMA
mentioned in the previous chapter. The values of μ are obtained from B.
P. C., those of the radial velocity (_W_) from the card catalogue in
Lund already described.

There are in all, in the sky, 20 stars having an apparent magnitude
brighter than 1m.5. The brightest of them is _Sirius_, which, owing to
its brilliancy and position, is visible to the whole civilized world. It
has a spectrum of the type A0 and hence a colour-index nearly equal to
0.0 (observations in Harvard give _c_ = +0.06). Its apparent magnitude
is -1m.6, nearly the same as that of Mars in his opposition. Its
absolute magnitude is -0m.3, _i.e._, fainter than the apparent
magnitude, from which we may conclude that it has a distance from us
smaller than one siriometer. We find, indeed, from the eighth column
that _r_ = 0.5 sir. The proper motion of Sirius is 1″.32 per year, which
is rather large but still not among the largest proper motions as will
be seen below. From the 11th column we find that Sirius is moving
towards us with a velocity of 1.6 sir./st. (= 7.6 km./sec.), a rather
small velocity. The third column shows that its right ascension is 6h
40m and its declination -16°. It lies in the square GD_7 and its
galactic coordinates are seen in the 5th and 6th columns.

The next brightest star is _Canopus_ or α Carinæ at the south sky. If we
might place absolute confidence in the value of _M_ (= -8.2) in the 12th
column this star would be, in reality, a much more imposing apparition
than Sirius itself. Remembering that the apparent magnitude of the moon,
according to §6, amounts to -11.6, we should find that Canopus, if
placed at a distance from us equal to that of Sirius (_r_ = 0.5 sir.),
would shine with a lustre equal to no less than a quarter of that of the
moon. It is not altogether astonishing that a fanciful astronomer should
have thought Canopus to be actually the central star in the whole
stellar system. We find, however, from column 8 that its supposed
distance is not less that 30 sir. We have already pointed out that
distances greater than 4 sir., when computed from annual parallaxes,
must generally be considered as rather uncertain. As the value of _M_
is intimately dependent on that of _r_ we must consider speculations
based on this value to be very vague. Another reason for a doubt about a
great value for the real luminosity of this star is found from its type
of spectrum which, according to the last column, is F0, a type which, as
will be seen, is seldom found among giant stars. A better support for a
large distance could on the other hand be found from the small proper
motion of this star. Sirius and Canopus are the only stars in the sky
having a negative value of the apparent visual magnitude.

Space will not permit us to go through this list star for star. We may
be satisfied with some general remarks.

In the fourth column is the galactic square. We call to mind that all
these squares have the same area, and that there is therefore the same
probability _a priori_ of finding a star in one of the squares as in
another. The squares GC and GD lie along the galactic equator (the Milky
Way). We find now from column 4 that of the 20 stars here considered
there are no less than 15 in the galactic equator squares and only 5
outside, instead of 10 in the galactic squares and 10 outside, as would
have been expected. The number of objects is, indeed, too small to allow
us to draw any cosmological conclusions from this distribution, but we
shall find in the following many similar instances regarding objects
that are principally accumulated along the Milky Way and are scanty at
the galactic poles. We shall find that in these cases we may _generally_
conclude from such a partition that we then have to do with objects
_situated far from the sun_, while objects that are uniformly
distributed on the sky lie relatively near us. It is easy to understand
that this conclusion is a consequence of the supposition, confirmed by
all star counts, that the stellar system extends much farther into space
along the Milky Way than in the direction of its poles.

If we could permit ourselves to draw conclusions from the small material
here under consideration, we should hence have reason to believe that
the bright stars lie relatively far from us. In other words we should
conclude that the bright stars seem to be bright to us not because of
their proximity but because of their large intrinsic luminosity. Column
8 really tends in this direction. Certainly the distances are not in
this case colossal, but they are nevertheless sufficient to show, in
some degree, this uneven partition of the bright stars on the sky. The
mean distance of these stars is as large as 7.5 sir. Only α Centauri,
Sirius, Procyon and Altair lie at a distance smaller than one
siriometer. Of the other stars there are two that lie as far as 30
siriometers from our system. These are the two giants Canopus and Rigel.
Even if, as has already been said, the distances of these stars may be
considered as rather uncertain, we must regard them as being rather

As column 8 shows that these stars are rather far from us, so we find
from column 12, that their absolute luminosity is rather large. The mean
absolute magnitude is, indeed, -2m.1. We shall find that only the
greatest and most luminous stars in the stellar system have a negative
value of the absolute magnitude.

The mean value of the proper motions of the bright stars amounts to
0″.56 per year and may be considered as rather great. We shall, indeed,
find that the mean proper motion of the stars down to the 6th magnitude
scarcely amounts to a tenth part of this value. On the other hand we
find from the table that the high value of this mean is chiefly due to
the influence of four of the stars which have a large proper motion,
namely Sirius, Arcturus, α Centauri and Procyon. The other stars have a
proper motion smaller than 1″ per year and for half the number of stars
the proper motion amounts to approximately 0″.05, indicating their
relatively great distance.

That the absolute velocity of these stars is, indeed, rather small may
be found from column 10, giving their radial velocity, which in the mean
amounts to only three siriometers per stellar year. From the discussion
below of the radial velocities of the stars we shall find that this is a
rather small figure. This fact is intimately bound up with the general
law in statistical mechanics, to which we return later, that stars with
large masses generally have a small velocity. We thus find in the radial
velocities fresh evidence, independent of the distance, that these
bright stars are giants among the stars in our stellar system.

We find all the principal spectral types represented among the bright
stars. To the helium stars (B) belong Rigel, Achernar, β Centauri,
Spica, Regulus and β Crucis. To the Sirius type (A) belong Sirius, Vega,
Altair, Fomalhaut and Deneb. To the Calcium type (F) Canopus and
Procyon. To the sun type (G) Capella and α Centauri. To the K-type
belong Arcturus, Aldebaran and Pollux and to the M-type the two red
stars Betelgeuze and Antares. Using the spectral indices as an
expression for the spectral types we find that the mean spectral index
of these stars is +1.1 corresponding to the spectral type F1.

31. _Stars with the greatest proper motion._ In table 3 I have collected
the stars having a proper motion greater than 3″ per year. The
designations are the same as in the preceding table, except that the
names of the stars are here taken from different catalogues.

In the astronomical literature of the last century we find the star 1830
Groombridge designed as that which possesses the greatest known proper
motion. It is now distanced by two other stars C. P. D. 5h.243
discovered in the year 1897 by KAPTEYN and INNES on the plates taken for
the Cape Photographic Durchmusterung, and BARNARD's star in Ophiuchus,
discovered 1916. The last-mentioned star, which possesses the greatest
proper motion now known, is very faint, being only of the 10th
magnitude, and lies at a distance of 0.40 sir. from our sun and is
hence, as will be found from table 5 the third nearest star for which we
know the distance. Its linear velocity is also very great, as we find
from column 10, and amounts to 19 sir./st. (= 90 km./sec.) in the
direction towards the sun. The absolute magnitude of this star is 11m.7
and it is, with the exception of one other, the very faintest star now
known. Its spectral type is Mb, a fact worth fixing in our memory, as
different reasons favour the belief that it is precisely the M-type that
contains the very faintest stars. Its apparent velocity (_i.e._, the
proper motion) is so great that the star in 1000 years moves 3°, or as
much as 6 times the diameter of the moon. For this star, as well as for
its nearest neighbours in the table, observations differing only by a
year are sufficient for an approximate determination of the value of the
proper motion, for which in other cases many tens of years are

Regarding the distribution of these stars in the sky we find that,
unlike the brightest stars, they are not concentrated along the Milky
Way. On the contrary we find only 6 in the galactic equator squares and
12 in the other squares. We shall not build up any conclusion on this
irregularity in the distribution, but supported by the general thesis of
the preceding paragraph we conclude only that these stars must be
relatively near us. This follows, indeed, directly from column 8, as not
less than eleven of these stars lie within one siriometer from our sun.
Their mean distance is 0.87 sir.



| 1|         2           |    3     |    4   |  5  |   6   |   7   |   8   |
|  |                     |           Position              |   Distance    |
|  | _Name_              |----------+--------+-----+-------+-------+-------+
|  |                     |   (αδ)    | Square | _l_ |  _b_  |  π   |  _r_  |
|  |                     |          |        |     |       |       | sir.  |
| 1|Barnards star        |(175204)  |  GC_12 | 358°| +12°  |0″.515 |  0.40 |
| 2|C. Z. 5h.243         |(0507{44})|  GE_7  | 218 | -35   | 0.319 |  0.65 |
| 3|Groom. 1830          |(114738)  |  GA_1  | 135 | +75   | 0.102 |  2.02 |
| 4|Lac. 9352            |(2259{36})|  GE_10 | 333 | -66   | 0.292 |  0.71 |
| 5|C. G. A. 32416       |(2359{37})|  GF_2  | 308 | -75   | 0.230 |  0.89 |
| 6|61 Cygni             |(210238)  |  GD_2  |  50 | - 7   | 0.311 |  0.66 |
| 7|Lal. 21185           |(105736)  |  GB_5  | 153 | +66   | 0.403 |  0.51 |
| 8|ε Indi               |(2155{57})|  GE_9  | 304 | -47   | 0.284 |  0.73 |
| 9|Lal. 21258           |(110044)  |  GB_4  | 135 | +64   | 0.203 |  1.02 |
|10|O^2 Eridani          |(0410{07})|  GE_5  | 168 | -36   | 0.174 |  1.19 |
|11|Proxima Centauri     |(1422{62})|  GD_10 | 281 | - 2   | 0.780 |  0.26 |
|12|Oe. A. 14320         |(1504{15})|  GB_9  | 314 | +35   | 0.035 |  5.90 |
|13|μ Cassiopeiæ         |(010154)  |  GD_4  |  93 | - 8   | 0.112 |  1.84 |
|14|α Centauri           |(1432{60})|  GD_10 | 284 | - 2   | 0.759 |  0.27 |
|15|Lac. 8760            |(2111{39})|  GE_10 | 332 | -44   | 0.248 |  0.83 |
|16|Lac. 1060            |(0315{43})|  GE_7  | 216 | -55   | 0.162 |  1.27 |
|17|Oe. A. 11677         |(111466)  |  GB_8  | 103 | +50   | 0.198 |  1.04 |
|18|Van Maanens star     |(004304)  |  GD_8  |  92 | -58   | 0.246 |  0.84 |
|  |                     |          |        |     |       |       | sir.  |
|  |   Mean              |   ..     |   ..   |     |  41°  |0″.298 |  0.87 |

| 1|         2           |   9  |   10   |    11   |    12   | 13 |  14  |
|  |                     |    Motion     |     Magnitude     | Spectrum  |
|  | _Name_              +------+--------+---------+---------+----+------+
|  |                     |  μ   |  _W_   |   _m_   |   _M_   |_Sp_| _m′_ |
|  |                     |      |sir./st.|         |         |    | _m′_ |
| 1|Barnards star        |10″.29|  -19   |    9m.7 |   +11m.7|Mb  |11.5  |
| 2|C. Z. 5h.243         |  8.75|  +51   |     9.2 |   +10.1 |K2  |10.6  |
| 3|Groom. 1830          |  7.06|  -20   |     6.5 |    +5.0 |G5  | 7.6  |
| 4|Lac. 9352            |  6.90|   +2   |     7.5 |    +8.2 |K   | 8.9  |
| 5|C. G. A. 32416       |  6.11|   +5   |     8.2 |    +8.5 |G   | 9.1  |
| 6|61 Cygni             |  5.27|  -13   |     5.6 |    +6.5 |K5  | 7.2  |
| 7|Lal. 21185           |  4.77|  -18   |     7.6 |    +9.1 |Mb  | 8.9  |
| 8|ε Indi               |  4.70|   -8   |     4.7 |    +5.4 |K5  | 6.3  |
| 9|Lal. 21258           |  4.47|  +14   |     8.5 |    +8.5 |Ma  |10.3  |
|10|O^2 Eridani          |  4.11|   -9   |     4.7 |    +4.3 |G5  | 5.8  |
|11|Proxima Centauri     |  3.85|   ..   |    11.0 |   +13.9 |..  |13.5  |
|12|Oe. A. 14320         |  3.75|  +61   |     9.0 |    +5.1 |G0  | 9.9  |
|13|μ Cassiopeiæ         |  3.73|  -21   |     5.7 |    +4.4 |G3  | 6.8  |
|14|α Centauri           |  3.68|   -5   |     0.3 |    +3.2 |G   | 1.2  |
|15|Lac. 8760            |  3.53|   +3   |     6.6 |    +7.0 |G   | 7.5  |
|16|Lac. 1060            |  3.05|  +18   |     5.6 |    +5.1 |G5  | 6.7  |
|17|Oe. A. 11677         |  3.03|   ..   |     9.2 |    +9.1 |Ma  |11.0  |
|18|Van Maanens star     |  3.01|   ..   |    12.3 |   +12.7 |F0  |12.9  |
|  |                     |      |sir./st.|         |         |    | _m′_ |
|  |   Mean              | 5″.00|   17.8 |    7m.3 |    +7m.6|G8  | 8.7  |

That the great proper motion does not depend alone on the proximity of
these stars is seen from column 10, giving the radial velocities. For
some of the stars (4) the radial velocity is for the present unknown,
but the others have, with few exceptions, a rather great velocity
amounting in the mean to 18 sir./st. (= 85 km./sec.), if no regard is
taken to the sign, a value nearly five times as great as the absolute
velocity of the sun. As this is only the component along the line of
sight, the absolute velocity is still greater, approximately equal to
the component velocity multiplied by √2. We conclude that the great
proper motions depend partly on the proximity, partly on the great
linear velocities of the stars. That both these attributes here really
cooperate may be seen from the absolute magnitudes (_M_).

The apparent and the absolute magnitudes are for these stars nearly
equal, the means for both been approximately 7m. This is a consequence
of the fact that the mean distance of these stars is equal to one
siriometer, at which distance _m_ and _M_, indeed, do coincide. We find
that these stars have a small luminosity and may be considered as
_dwarf_ stars. According to the general law of statistical mechanics
already mentioned small bodies upon an average have a great absolute
velocity, as we have, indeed, already found from the observed radial
velocities of these stars.

As to the spectral type, the stars with great proper motions are all
yellow or red stars. The mean spectral index is +2.8, corresponding to
the type G8. If the stars of different types are put together we get the

    _Type_    _Number_       _Mean value of M_
      G         8                 5.3
      K         4                 7.5
      M         4                 9.6

We conclude that, at least for these stars, the mean value of the
absolute magnitude increases with the spectral index. This conclusion,
however, is not generally valid.

32. _Stars with the greatest radial velocities._ There are some kinds of
nebulae for which very large values of the radial velocities have been
found. With these we shall not for the present deal, but shall confine
ourselves to the stars. The greatest radial velocity hitherto found is
possessed by the star (040822) of the eighth magnitude in the
constellation Perseus, which retires from us with a velocity of 72
sir./st. or 341 km./sec. The nearest velocity is that of the star
(010361) which approaches us with approximately the same velocity. The
following table contains all stars with a radial velocity greater than
20 sir./st. (= 94.8 km./sec.). It is based on the catalogue of VOUTE
mentioned above.

Regarding their distribution in the sky we find 11 in the galactic
equator squares and 7 outside. A large radial velocity seems therefore
to be a galactic phenomenon and to be correlated to a great distance
from us. Of the 18 stars in consideration there is only one at a
distance smaller than one siriometer and 2 at a distance smaller than 4
siriometers. Among the nearer ones we find the star (050744), identical
with C. P. D. 5h.243, which was the “second” star with great proper
motion. These stars have simultaneously the greatest proper motion and
very great linear velocity. Generally we find from column 9 that these
stars with large radial velocity possess also a large proper motion. The
mean value of the proper motions amounts to 1″.34, a very high value.

In the table we find no star with great apparent luminosity. The
brightest is the 10th star in the table which has the magnitude 5.1. The
mean apparent magnitude is 7.7. As to the absolute magnitude (_M_) we
see that most of these speedy stars, as well as the stars with great
proper motions in table 3, have a rather great _positive_ magnitude and
thus are absolutely faint stars, though they perhaps may not be directly
considered as dwarf stars. Their mean absolute magnitude is +3.0.

Regarding the spectrum we find that these stars generally belong to the
yellow or red types (G, K, M), but there are 6 F-stars and, curiously
enough, two A-stars. After the designation of their type (A2 and A3) is
the letter _p_ (= peculiar), indicating that the spectrum in some
respect differs from the usual appearance of the spectrum of this type.
In the present case the peculiarity consists in the fact that a line of
the wave-length 448.1, which emanates from magnesium and which we may
find on plate III in the spectrum of Sirius, does not occur in the
spectrum of these stars, though the spectrum has otherwise the same
appearance as in the case of the Sirius stars. There is reason to
suppose that the absence of this line indicates a low power of radiation
(low temperature) in these stars (compare ADAMS).



| 1|         2           |    3     |    4   |  5  |   6   |   7   |   8   |
|  |                     |           Position              |   Distance    |
|  | _Name_              |----------+--------+-----+-------+-------+-------+
|  |                     |  (αδ)    | Square | _l_ |  _b_  |   π   |  _r_  |
|  |                     |          |        |     |       |       | sir.  |
| 1|A. G. Berlin 1366    |(040822)  |  GD_5  | 141°| -20°  |0″.007 | 30.8  |
| 2|Lal. 1966            |(010361)  |  GD_4  |  93 | - 2   | 0.016 | 12.9  |
| 3|A. Oe. 14320         |(1504{15})|  GB_9  | 314 | +35   | 0.035 |  5.9  |
| 4|C. Z. 5h.243         |(0507{44})|  GE_7  | 218 | -35   | 0.319 |  0.6  |
| 5|Lal. 15290           |(074730)  |  GC_6  | 158 | +26   | 0.023 |  9.0  |
| 6|53 Cassiop.          |(015563)  |  GC_4  |  98 | + 2   |  ..   |  ..   |
| 7|A. G. Berlin 1866    |(055719)  |  GD_6  | 159 | - 2   | 0.021 |  9.8  |
| 8|W Lyræ               |(181136)  |  GC_2  |  31 | +21   |  ..   |  ..   |
| 9|Boss 1511            |(0559{26})|  GD_7  | 200 | -20   | 0.012 | 17.0  |
|10|ω Pavonis            |(1849{60})|  GD_11 | 304 | -24   |  ..   |  ..   |
|11|A. Oe. 20452         |(2017{21})|  GE_10 | 351 | -31   | 0.015 | 13.5  |
|12|Lal. 28607           |(1537{10})|  GB_10 | 325 | +34   | 0.033 |  6.2  |
|13|A. G. Leiden 5734    |(161132)  |  GB_1  |  21 | +45   | 0.002 | 89.2  |
|14|Lal. 37120           |(192932)  |  GC_2  |  33 | + 6   | 0.050 |  4.1  |
|15|Lal. 27274           |(1454{21})|  GB_9  | 308 | +34   | 0.013 | 16.2  |
|16|Lal. 5761            |(030225)  |  GD_5  | 126 | -28   | 0.039 |  5.1  |
|17|W. B. 17h.517        |(172906)  |  GC_12 | 358 | +20   | 0.014 | 14.1  |
|18|Lal. 23995           |(1247{17})|  GB_8  | 271 | +46   | 0.012 | 17.0  |
|  |                     |          |        |     |       |       | sir.  |
|  |   Mean              |    ..    |   ..   |     |  23°.9|0″.041 | 16.7  |

| 1|         2           |   9  |   10   |    11   |    12   | 13 |  14  |
|  |                     |    Motion     |     Magnitude     | Spectrum  |
|  | _Name_              +------+--------+---------+---------+----+------+
|  |                     |   μ  |  _W_   |   _m_   |   _M_   |_Sp_| _m′_ |
|  |                     |      |sir./st.|         |         |    | _m′_ |
| 1|A. G. Berlin 1366    | 0″.54|  +72   |  8m.9   |  +1m.4  |F0  | 9.4  |
| 2|Lal. 1966            |  0.64|  -69   |   7.9   |   +2.3  |F3  | 8.5  |
| 3|A. Oe. 14320         |  3.75|  +61   |   9.0   |   +5.1  |G0  | 9.9  |
| 4|C. Z. 5h.243         |  8.75|  +51   |   9.2   |  +10.1  |K2  |10.6  |
| 5|Lal. 15290           |  1.96|  -51   |   8.2   |   +3.4  |G0  | 9.1  |
| 6|53 Cassiop.          |  0.01|  -44   |   5.6   |    ..   |B8  | 5.5  |
| 7|A. G. Berlin 1866    |  0.76|  -40   |   9.0   |   +4.0  |F0  | 9.9  |
| 8|W Lyræ               | ..   |  -39   |   var.  |    ..   |Md  | var. |
| 9|Boss 1511            |  0.10|  +39   |   5.2   |   -1.0  |G5  | 6.4  |
|10|ω Pavonis            |  0.14|  +38   |   5.1   |    ..   |K   | 6.5  |
|11|A. Oe. 20452         |  1.18|  -38   |   8.1   |   +2.4  |G8p | 9.4  |
|12|Lal. 28607           |  1.18|  -36   |   7.3   |   +3.3  |A2p | 7.4  |
|13|A. G. Leiden 5734    |  0.04|  -35   |   8.3   |   -1.5  |K4  | 9.9  |
|14|Lal. 37120           |  0.52|  -34   |   6.6   |   +3.5  |G2  | 7.6  |
|15|Lal. 27274           |  0.79|  +34   |   8.3   |   +2.2  |F4  | 8.9  |
|16|Lal. 5761            |  0.86|  -32   |   8.0   |   +4.4  |A3p | 8.1  |
|17|W. B. 17h.517        |  0.63|  -31   |   8.6   |   +2.8  |F1  | 9.1  |
|18|Lal. 23995           |  0.88|  +30   |   8.2   |   +2.0  |F3  | 8.8  |
|  |                     |      |sir./st.|         |         |    | _m′_ |
|  |   Mean              | 1″.34|   16.7 |  7m.7   |  +3m.0  |F9  | 8.5  |

33. _The nearest stars._ The star α in Centaurus was long considered as
the nearest of all stars. It has a parallax of 0″.75, corresponding to a
distance of 0.27 siriometers (= 4.26 light years). This distance is
obtained from the annual parallax with great accuracy, and the result is
moreover confirmed in another way (from the study of the orbit of the
companion of α Centauri). In the year 1916 INNES discovered at the
observatory of Johannesburg in the Transvaal a star of the 10th
magnitude, which seems to follow α Centauri in its path in the heavens,
and which, in any case, lies at the same distance from the earth, or
somewhat nearer. It is not possible at present to decide with accuracy
whether _Proxima Centauri_--as the star is called by INNES--or α
Centauri is our nearest neighbour. Then comes BARNARD's star (175204),
whose large proper motion we have already mentioned. As No. 5 we find
Sirius, as No. 8 Procyon, as No. 21 Altair. The others are of the third
magnitude or fainter. No. 10--61 Cygni--is especially interesting, being
the first star for which the astronomers, after long and painful
endeavours in vain, have succeeded in determining the distance with the
help of the annual parallax (BESSEL 1841).

From column 4 we find that the distribution of these stars on the sky is
tolerably uniform, as might have been predicted. All these stars have a
large proper motion, this being in the mean 3″.42 per year. This was a
priori to be expected from their great proximity. The radial velocity
is, numerically, greater than could have been supposed. This fact is
probably associated with the generally small mass of these stars.

Their apparent magnitude is upon an average 6.3. The brightest of the
near stars is Sirius (_m_ = -1.6), the faintest Proxima Centauri (_m_ =
11). Through the systematic researches of the astronomers we may be sure
that no bright stars exist at a distance smaller than one siriometer,
for which the distance is not already known and well determined. The
following table contains without doubt--we may call them briefly all
_near_ stars--all stars within one siriometer from us with an apparent
magnitude brighter than 6m (the table has 8 such stars), and probably
also all near stars brighter than 7m (10 stars), or even all brighter
than the eighth magnitude (the table has 13 such stars and two near the
limit). Regarding the stars of the eighth magnitude or fainter no
systematic investigations of the annual parallax have been made and
among these stars we may get from time to time a new star belonging to
the siriometer sphere in the neighbourhood of the sun. To determine
the total number of stars within this sphere is one of the fundamental
problems in stellar statistics, and to this question I shall return



| 1|         2            |    3     |    4   |  5  |   6   |   7   |   8   |
|  |                      |           Position              |   Distance    |
|  | _Name_               |----------+--------+-----+-------+-------+-------+
|  |                      |   (αδ)   | Square | _l_ |  _b_  |   π   | _r_   |
|  |                      |          |        |     |       |       | sir.  |
| 1|Proxima Centauri      |(1422{62})|  GD_10 | 281°| - 2°  |0″.780 |  0.26 |
| 2|α Centauri            |(1432{60})|  GD_10 | 284 | - 2   | 0.759 |  0.27 |
| 3|Barnards p. m. star   |(175204)  |  GC_12 | 358 | +12   | 0.515 |  0.40 |
| 4|Lal. 21185            |(105736)  |  GB_5  | 153 | +66   | 0.403 |  0.51 |
| 5|Sirius                |(0640{16})|  GD_7  | 195 | - 8   | 0.376 |  0.55 |
| 6|            ..        |(1113{57})|  GC_6  | 158 | + 3   | 0.337 |  0.60 |
| 7|τ Ceti                |(0139{16})|  GF_1  | 144 | -74   | 0.334 |  0.62 |
| 8|Procyon               |(073405)  |  GC_7  | 182 | +14   | 0.324 |  0.64 |
| 9|C. Z. 5h.243          |(0507{44})|  GE_7  | 218 | -35   | 0.319 |  0.65 |
|10|61 Cygni              |(210238)  |  GD_2  |  50 | - 7   | 0.311 |  0.66 |
|11|Lal. 26481            |(1425{15})|  GB_9  | 124 | -40   | 0.311 |  0.66 |
|12|ε Eridani             |(0328{09})|  GE_5  | 153 | -42   | 0.295 |  0.70 |
|13|Lac. 9352             |(2259{36})|  GE_10 | 333 | -66   | 0.292 |  0.71 |
|14|Pos. Med. 2164        |(184159)  |  GC_2  |  56 | +24   | 0.292 |  0.71 |
|15|ε Indi                |(215557)  |  GE_9  | 304 | -47   | 0.284 |  0.73 |
|16|Groom. 34             |(001243)  |  GD_3  |  84 | -20   | 0.281 |  0.73 |
|17|Oe. A. 17415          |(173768)  |  GC_8  |  65 | +32   | 0.268 |  0.77 |
|18|Krüger 60             |(222457)  |  GC_3  |  72 |   0   | 0.256 |  0.81 |
|19|Lac. 8760             |(2111{39})|  GE_10 | 332 | -44   | 0.248 |  0.88 |
|20|van Maanens p. m. star|(004304)  |  GE_3  |  92 | -58   | 0.246 |  0.84 |
|21|Altair                |(194508)  |  GD_1  |  15 | -10   | 0.238 |  0.87 |
|22|C. G. A. 32416        |(2359{37})|  GF_2  | 308 | -75   | 0.230 |  0.89 |
|23|Bradley 1584          |(1129{32})|  GC_6  | 252 | +28   | 0.216 |  0.95 |
|  |                      |          |        |     |       |       | sir.  |
|  |   Mean               |   ..     |   ..   |  .. |  30°.8|0″.344 |  0.67 |

| 1|         2             |   9  |   10   |    11   |    12   | 13 |  14  |
|  |                       |    Motion     |     Magnitude     | Spectrum  |
|  | _Name_                +------+--------+---------+---------+----+------+
|  |                       | μ |  _W_   |   _m_   |   _M_   |_Sp_| _m′_ |
|  |                       |      |sir./st.|         |         |    | _m′_ |
| 1|Proxima Centauri       | 3″.85|   ..   | 11m.0   | +13m.9  |..  |13.5  |
| 2|α Centauri             |  3.68|  - 5   |   0.33  |  + 3.2  |G   | 1.25 |
| 3|Barnards p. m. star    | 10.29|  -19   |   9.7   |  +11.7  |Mb  |11.5  |
| 4|Lal. 21185             |  4.77|  -18   |   7.6   |  + 9.1  |Mb  | 8.9  |
| 5|Sirius                 |  1.32|  - 2   |  -1.58  |  - 0.3  |A   |-1.58 |
| 6|            ..         |  2.72|   ..   |  ..     |  ..     |..  |12.5  |
| 7|τ Ceti                 |  1.92|  - 3   |   3.6   |  + 4.6  |K0  | 4.6  |
| 8|Procyon                |  1.24|  - 1   |   0.48  |  + 1.5  |F5  | 0.90 |
| 9|C. Z. 5h.243           |  8.75|  +51   |   9.2   |  +10.1  |K2  |10.6  |
|10|61 Cygni               |  5.27|  -13   |   5.6   |  + 6.5  |K5  | 7.2  |
|11|Lal. 26481             |  0.47|   ..   |   7.8   |  + 8.7  |G5  | 8.9  |
|12|ε Eridani              |  0.97|  + 3   |   3.8   |  + 4.6  |K0  | 4.8  |
|13|Lac. 9352              |  6.90|  + 2   |   7.5   |  + 8.2  |K   | 8.9  |
|14|Pos. Med. 2164         |  2.28|   ..   |   8.9   |  + 9.6  |K   |10.3  |
|15|ε Indi                 |  4.70|  - 8   |   4.7   |  + 5.4  |K5  | 6.3  |
|16|Groom. 34              |  2.89|  + 1   |   8.1   |  + 8.8  |Ma  | 9.5  |
|17|Oe. A. 17415           |  1.30|   ..   |   9.1   |  + 9.7  |K   |10.5  |
|18|Krüger 60              |  0.94|   ..   |   9.2   |  + 9.6  |K5  |10.8  |
|19|Lac. 8760              |  3.53|  + 3   |   6.6   |  + 7.0  |G   | 7.5  |
|20|van Maanens p. m. star |  3.01|   ..   |  12.3   |  +12.7  |F0  |12.9  |
|21|Altair                 |  0.66|  - 7   |   0.9   |  + 1.2  |A5  | 1.12 |
|22|C. G. A. 32416         |  6.11|  + 5   |   8.2   |  + 8.5  |G   | 9.1  |
|23|Bradley 1584           |  1.06|  - 5   |   6.1   |  + 6.2  |G   | 6.9  |
|  |                       |      |sir./st.|         |         |    | _m′_ |
|  |   Mean                | 3″.42|    9.1 |  6m.3   |  +7m.3  |G6  | 7.5  |

The mean absolute magnitude of the near stars is distributed in the
following way:--

    _M_         0 1 3 4 5 6 7 8 9 10 11 12 13
    Number      1 2 1 2 1 2 1 4 4 1  1  1  1.

What is the absolute magnitude of the near stars that are not contained
in table? Evidently they must principally be faint stars. We may go
further and answer that _all stars with an absolute magnitude brighter
than 6m_ must be contained in this list. For if _M_ is equal to 6 or
brighter, _m_ must be brighter than 6m, if the star is nearer than one
siriometer. But we have assumed that all stars apparently brighter than
6m are known and are contained in the list. Hence also all stars
_absolutely_ brighter than 6m must be found in table 5. We conclude that
the number of stars having an absolute magnitude brighter than 6m
amounts to 8.

If, finally, the spectral type of the near stars is considered, we find
from the last column of the table that these stars are distributed in
the following way:--

    Spectral type   B A F G K M
    Number          0 2 2 5 9 3.

For two of the stars the spectrum is for the present unknown.

We find that the number of stars increases with the spectral index. The
unknown stars in the siriometer sphere belong probably, in the main, to
the red types.

If we now seek to form a conception of the _total_ number in this sphere
we may proceed in different ways. EDDINGTON, in his “Stellar movements”,
to which I refer the reader, has used the proper motions as a scale of
calculation, and has found that we may expect to find in all 32 stars in
this sphere, confining ourselves to stars apparently brighter than the
magnitude 9m.5. This makes 8 stars per cub. sir.

We may attack the problem in other ways. A very rough method which,
however, is not without importance, is the following. Let us suppose
that the Galaxy in the direction of the Milky Way has an extension of
1000 siriometers and in the direction of the poles of the Milky Way an
extension of 50 sir. We have later to return to the fuller discussion of
this extension. For the present it is sufficient to assume these values.
The whole system of the Galaxy then has a volume of 200 million cubic
siriometers. Suppose further that the total number of stars in the
Galaxy would amount to 1000 millions, a value to which we shall also
return in a following chapter. Then we conclude that the average number
of stars per cubic siriometer would amount to 5. This supposes that the
density of the stars in each part of the Galaxy is the same. But the sun
lies rather near the centre of the system, where the density is
(considerably) greater than the average density. A calculation, which
will be found in the mathematical part of these lectures, shows that the
density in the centre amounts to approximately 16 times the average
density, giving 80 stars per cubic siriometer in the neighbourhood of
the sun (and of the centre). A sphere having a radius of one siriometer
has a volume of 4 cubic siriometers, so that we obtain in this way 320
stars in all, within a sphere with a radius of one siriometer. For
different reasons it is probable that this number is rather too great
than too small, and we may perhaps estimate the total number to be
something like 200 stars, of which more than a tenth is now known to the

We may also arrive at an evaluation of this number by proceeding from
the number of stars of different apparent or absolute magnitudes. This
latter way is the most simple. We shall find in a later paragraph that
the absolute magnitudes which are now known differ between -8 and +13.
But from mathematical statistics it is proved that the total range of a
statistical series amounts upon an average to approximately 6 times the
dispersion of the series. Hence we conclude that the dispersion (σ) of
the absolute magnitudes of the stars has approximately the value 3 (we
should obtain σ = [13 + 8] : 6 = 3.5, but for large numbers of
individuals the total range may amount to more than 6 σ).

As, further, the number of stars per cubic siriometer with an absolute
magnitude brighter than 6 is known (we have obtained 8 : 4 = 2 stars per
cubic siriometer brighter than 6m), we get a relation between the total
number of stars per cubic siriometer (_D_0_) and the mean absolute
magnitude (_M_0_) of the stars, so that _D_0_ can be obtained, as soon
as _M_0_ is known. The computation of _M_0_ is rather difficult, and is
discussed in a following chapter. Supposing, for the moment, _M_0_ = 10
we get for _D_0_ the value 22, corresponding to a number of 90 stars
within a distance of one siriometer from the sun. We should then know a
fifth part of these stars.

34. _Parallax stars._ In §22 I have paid attention to the now available
catalogues of stars with known annual parallax. The most extensive of
these catalogues is that of WALKEY, containing measured parallaxes of
625 stars. For a great many of these stars the value of the parallax
measured must however be considered as rather uncertain, and I have
pointed out that only for such stars as have a parallax greater than
0″.04 (or a distance smaller than 5 siriometers) may the measured
parallax be considered as reliable, as least generally speaking. The
effective number of parallax stars is therefore essentially reduced.
Indirectly it is nevertheless possible to get a relatively large
catalogue of parallax stars with the help of the ingenious spectroscopic
method of ADAMS, which permits us to determine the absolute magnitude,
and therefore also the distance, of even farther stars through an
examination of the relative intensity of certain lines in the stellar
spectra. It may be that the method is not yet as firmly based as it
should be,[15] but there is every reason to believe that the course
taken is the right one and that the catalogue published by ADAMS of 500
parallax stars in Contrib. from Mount Wilson, 142, already gives a more
complete material than the catalogues of directly measured parallaxes. I
give here a short resumé of the attributes of the parallax stars in this

The catalogue of ADAMS embraces stars of the spectral types F, G, K and
M. In order to complete this material by parallaxes of blue stars I add
from the catalogue of WALKEY those stars in his catalogue that belong to
the spectral types B and A, confining myself to stars for which the
parallax may be considered as rather reliable. There are in all 61 such
stars, so that a sum of 561 stars with known distance is to be

For all these stars we know _m_ and _M_ and for the great part of them
also the proper motion μ. We can therefore for each spectral type
compute the mean values and the dispersion of these attributes. We thus
get the following table, in which I confine myself to the mean values of
the attributes.



|Sp.|Number |  _m_  |  _M_  |   μ   |
| B |  15   | +2.03 | -1.67 | 0″.05 |
| A |  46   | +3.40 | +0.64 | 0.21  |
| F | 125   | +5.60 | +2.10 | 0.40  |
| G | 179   | +5.77 | +1.68 | 0.51  |
| K | 184   | +6.17 | +2.31 | 0.53  |
| M |  42   | +6.02 | +2.30 | 0.82  |

We shall later consider all parallax stars taken together. We find from
table 6 that the apparent magnitude, as well as the absolute magnitude,
is approximately the same for all yellow and red stars and even for the
stars of type F, the apparent magnitude being approximately equal to +6m
and the absolute magnitude equal to +2m. For type B we find the mean
value of M to be -1m.7 and for type A we find M = +0m.6. The proper
motion also varies in the same way, being for F, G, K, M approximately
0″.5 and for B and A 0″.1. As to the mean values of _M_ and μ we cannot
draw distinct conclusions from this material, because the parallax stars
are selected in a certain way which essentially influences these mean
values, as will be more fully discussed below. The most interesting
conclusion to be drawn from the parallax stars is obtained from their
distribution over different values of _M_. In the memoir referred to,
ADAMS has obtained the following table (somewhat differently arranged
from the table of ADAMS),[16] which gives the number of parallax stars
for different values of the absolute magnitude for different spectral

A glance at this table is sufficient to indicate a singular and well
pronounced property in these frequency distributions. We find, indeed,
that in the types G, K and M the frequency curves are evidently
resolvable into two simple curves of distribution. In all these types we
may distinguish between a bright group and a faint group. With a
terminology proposed by HERTZSPRUNG the former group is said to consist
of _giant_ stars, the latter group of _dwarf_ stars. Even in the stars
of type F this division may be suggested. This distinction is still more
pronounced in the graphical representation given in figures (plate IV).



|       |    |    |     |     |     |     ||      |
|   M   |  B |  A |   F |   G |   K |   M || All  |
|       |    |    |     |     |     |     ||      |
|  - 4  | .. | .. |  .. |  .. |  .. |   1 ||  ..  |
|  - 3  | .. | .. |  .. |  .. |  .. |  .. ||  ..  |
|  - 2  |  1 |  4 |   1 |   7 |  .. |   2 ||  15  |
|  - 1  |  2 |  7 |   7 |  28 |  15 |   4 ||  63  |
|  - 0  |  3 | 10 |   6 |  32 |  40 |  10 ||  91  |
|  + 0  |  1 | 11 |   6 |   7 |  14 |  11 ||  50  |
|  + 1  |  1 |  3 |  20 |   9 |   4 |   1 ||  38  |
|  + 2  | .. |  5 |  48 |  26 |  .. |   1 ||  80  |
|  + 3  | .. |  1 |  32 |  36 |   2 |  .. ||  71  |
|  + 4  | .. |  1 |   5 |  25 |  25 |  .. ||  56  |
|  + 5  | .. |  1 |  .. |   6 |  25 |  .. ||  32  |
|  + 6  | .. |  2 |  .. |   3 |  10 |  .. ||  15  |
|  + 7  | .. |  1 |  .. |  .. |  14 |  .. ||  15  |
|  + 8  | .. | .. |  .. |  .. |   3 |   7 ||  10  |
|  + 9  | .. | .. |  .. |  .. |   2 |   4 ||   6  |
|  +10  | .. | .. |  .. |  .. |  .. |  .. ||  ..  |
|  +11  | .. | .. |  .. |  .. |  .. |   1 ||   1  |
| Total |  8 | 46 | 125 | 179 | 154 |  42 || 554  |

In the distribution of all the parallax stars we once more find a
similar bipartition of the stars. Arguing from these statistics some
astronomers have put forward the theory that the stars in space are
divided into two classes, which are not in reality closely related. The
one class consists of intensely luminous stars and the other of feeble
stars, with little or no transition between the two classes. If the
parallax stars are arranged according to their apparent proper motion,
or even according to their absolute proper motion, a similar bipartition
is revealed in their frequency distribution.

Nevertheless the bipartition of the stars into two such distinct classes
must be considered as vague and doubtful. Such an _apparent_
bipartition is, indeed, necessary in all statistics as soon as
individuals are selected from a given population in such a manner as the
parallax stars are selected from the stars in space. Let us consider
three attributes, say _A_, _B_ and _C_, of the individuals of a
population and suppose that the attribute _C_ is _positively_ correlated
to the attributes _A_ and _B_, so that to great or small values of _A_
or _B_ correspond respectively great or small values of _C_. Now if the
individuals in the population are statistically selected in such a way
that we choose out individuals having great values of the attributes _A_
and small values of the attribute _B_, then we get a statistical series
regarding the attribute _C_, which consists of two seemingly distinct
normal frequency distributions. It is in like manner, however, that the
parallax stars are selected. The reason for this selection is the
following. The annual parallax can only be determined for near stars,
nearer than, say, 5 siriometers. The direct picking out of these stars
is not possible. The astronomers have therefore attacked the problem in
the following way. The near stars must, on account of their proximity,
be relatively brighter than other stars and secondly possess greater
proper motions than those. Therefore parallax observations are
essentially limited to (1) bright stars, (2) stars with great proper
motions. Hence the selected attributes of the stars are _m_ and μ. But
_m_ and μ are both positively correlated to _M_. By the selection of
stars with small _m_ and great μ we get a series of stars which
regarding the attribute _M_ seem to be divided into two distinct

The distribution of the parallax stars gives us no reason to believe
that the stars of the types K and M are divided into the two supposed
classes. There is on the whole no reason to suppose the existence at all
of classes of giant and dwarf stars, not any more than a classification
of this kind can be made regarding the height of the men in a
population. What may be statistically concluded from the distribution of
the absolute magnitudes of the parallax stars is only that the
_dispersion_ in _M_ is increased at the transition from blue to yellow
or red stars. The filling up of the gap between the “dwarfs” and the
“giants” will probably be performed according as our knowledge of the
distance of the stars is extended, where, however, not the annual
parallax but other methods of measuring the distance must be employed.



| 1|         2           |    3     |    4   |  5  |   6   |   7   |   8   |
|  |                     |             Position            |   Distance    |
|  | _Name_              |----------+--------+-----+-------+-------+-------+
|  |                     |    (αδ)  | Square | _l_ |  _b_  |   π   | _r_   |
|  |                     |          |        |     |       |       | sir.  |
| 1|Proxima Centauri     |(1422{62})|  GD_10 | 281°| - 2°  |0″.780 |  0.26 |
| 2|van Maanens star     |(004304)  |  GE_8  |  92 | -58   | 0.246 |  0.84 |
| 3|Barnards star        |(175204)  |  GC_12 | 358 | +12   | 0.515 |  0.40 |
| 4|17 Lyræ C            |(190332)  |  GC_2  |  31 | +10   | 0.128 |  1.60 |
| 5|C. Z. 5h.243         |(0507{44})|  GE_7  | 218 | -35   | 0.319 |  0.65 |
| 6|Gron. 19 VIII 234    |(161839)  |  GB_1  |  29 | +44   | 0.162 |  1.27 |
| 7|Oe. A. 17415         |(173768)  |  GB_8  |  65 | +32   | 0.268 |  0.77 |
| 8|Gron. 19 VII 20      |(162148)  |  GB_2  |  41 | +43   | 0.133 |  1.55 |
| 9|Pos. Med. 2164       |(184159)  |  GC_2  |  56 | +24   | 0.292 |  0.71 |
|10|Krüger 60            |(222457)  |  GC_8  |  72 |   0   | 0.256 |  0.81 |
|11|B. D. +56°532        |(021256)  |  GD_8  | 103 | - 4   | 0.195 |  1.06 |
|12|B. D. +55°581        |(021356)  |  GD_8  | 103 | - 4   | 0.185 |  1.12 |
|13|Gron. 19 VIII 48     |(160438)  |  GB_1  |  27 | +46   | 0.091 |  2.27 |
|14|Lal. 21185           |(105736)  |  GB_5  | 153 | +66   | 0.403 |  0.51 |
|15|Oe. A. 11677         |(111466)  |  GB_3  | 103 | +50   | 0.198 |  1.04 |
|16|Walkey 653           |(155359)  |  GB_2  |  57 | +45   | 0.175 |  1.18 |
|17|Yerkes parallax star |(021243)  |  GD_8  | 107 | -16   | 0.045 |  4.58 |
|18|B. D. +56°537        |(021256)  |  GD_8  | 103 | - 4   | 0.175 |  1.18 |
|19|Gron. 19 VI 266      |(062084)  |  GC_3  |  97 | +27   | 0.071 |  2.80 |
|  |                     |          |        |     |       |       | sir.  |
|  |   Mean              |   ..     |   ..   |  .. |  27°.5|0″.244 |  0.99 |

| 1|         2           |   9  |   10   |    11   |    12   | 13 |  14  |
|  |                     |    Motion     |     Magnitude     | Spectrum  |
|  | _Name_              +------+--------+---------+---------+----+------+
|  |                     |   μ  |  _W_   |   _m_   |   _M_   |_Sp_| _m′_ |
|  |                     |      |sir./st.|         |         |    | _m′_ |
| 1|Proxima Centauri     | 3″.85|   ..   | 11m.0    |+13m.9  |..  |13.5  |
| 2|van Maanens star     |  3.01|   ..   |  12.3   |  +12.7  |F0  |12.95 |
| 3|Barnards star        | 10.29|  -19   |   9.7   |  +11.7  |Mb  | 8.9  |
| 4|17 Lyræ C            |  1.75|   ..   |  11.3   |  +10.3  |..  |12.5  |
| 5|C. Z. 5h.243         |  8.75|  +51   |   9.2   |  +10.1  |K2  |10.68 |
| 6|Gron. 19 VIII 234    |  0.12|   ..   |  10.3   |  + 9.8  |..  |  ..  |
| 7|Oe. A. 17415         |  1.30|   ..   |   9.1   |  + 9.7  |K   |10.5  |
| 8|Gron. 19 VII 20      |  1.22|   ..   |  10.5   |  + 9.6  |..  |  ..0 |
| 9|Pos. Med. 2164       |  2.28|   ..   |   8.9   |  + 9.6  |K   |10.3  |
|10|Krüger 60            |  0.94|   ..   |   9.2   |  + 9.6  |K5  |10.8  |
|11|B. D. +56°532        |   .. |   ..   |   9.5   |  + 9.4  |..  |  ..  |
|12|B. D. +55°581        |   .. |   ..   |   9.4   |  + 9.2  |G5  |10.2  |
|13|Gron. 19 VIII 48     |  0.12|   ..   |  11.1   |  + 9.3  |..  |  ..  |
|14|Lal. 21185           |  4.77|  -18   |   7.6   |  + 9.1  |Mb  | 8.9  |
|15|Oe. A. 11677         |  3.03|   ..   |   9.2   |  + 9.1  |Ma  |11.0  |
|16|Walkey 653           |   .. |   ..   |   9.5   |  + 9.1  |..  |  ..  |
|17|Yerkes parallax star |   .. |   ..   |  12.4   |  + 9.1  |..  |  ..  |
|18|B. D. +56°537        |   .. |   ..   |   9.4   |  + 9.0  |..  |  ..  |
|19|Gron. 19 VI 266      |  0.09|   ..   |  11.3   |  + 9.0  |..  |  ..  |
|  |                     |      |sir./st.|         |         |    | _m′_ |
|  |   Mean              | 2″.96|   29.3 | 10m.0   |  +9m.9  |K1  |10.9  |

Regarding the absolute brightness of the stars we may draw some
conclusions of interest. We find from table 7 that the absolute
magnitude of the parallax stars varies between -4 and +11, the extreme
stars being of type M. The absolutely brightest stars have a rather
great distance from us and their absolute magnitude is badly determined.
The brightest star in the table is Antares with _M_ = -4.6, which value
is based on the parallax 0″.014 found by ADAMS. So small a parallax
value is of little reliability when it is directly computed from annual
parallax observations, but is more trustworthy when derived with the
spectroscopic method of ADAMS. It is probable from a discussion of the
_B_-stars, to which we return in a later chapter, that the absolutely
brightest stars have a magnitude of the order -5m or -6m. If the
parallaxes smaller than 0″.01 were taken into account we should find that
Canopus would represent the absolutely brightest star, having _M_ =
-8.17, and next to it we should find RIGEL, having _M_ = -6.97, but both
these values are based on an annual parallax equal to 0″.007, which is
too small to allow of an estimation of the real value of the absolute

If on the contrary the _absolutely faintest_ stars be considered, the
parallax stars give more trustworthy results. Here we have only to do
with near stars for which the annual parallax is well determined. In
table 8 I give a list of those parallax stars that have an absolute
magnitude greater than 9m.

There are in all 19 such stars. The faintest of all known stars is
INNES' star “Proxima Centauri” with _M_ = 13.9. The third star is
BARNARD's star with _M_ = 11.7, both being, together with α Centauri,
also the nearest of all known stars. The mean distance of all the faint
stars is 1.0 sir.

There is no reason to believe that the limit of the absolute magnitude
of the faint stars is found from these faint parallax stars:--Certainly
there are many stars in space with _M_ > 13m and the mean value of _M_,
for all stars in the Galaxy, is probably not far from the absolute value
of the faint parallax stars in this table. This problem will be
discussed in a later part of these lectures.


[Footnote 15: Compare ADAMS' memoirs in the Contributions from Mount

[Footnote 16: The first line gives the stars of an absolute magnitude
between -4.9 and -4.0, the second those between -3.9 and -3.0, &c. The
stars of type B and A are from WALKEY's catalogue.]

[Illustration: PLATE I.


[Illustration: PLATE II.

_Squares and Constellations._]

[Illustration: PLATE III.

_The Harvard Classification of Stellar Spectra._]

[Illustration: Plate IV.

_Distribution of the parallax stars over different absolute


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       *       *       *       *       *

[Transcriber's Note: The following corrections have been made to the
original text.

Page 4: "Terrestial distances" changed to "Terrestrial distances"

Page 9: "we must chose," changed to "we must choose,"

Page 12: "acromasie" changed to "achromatism"

Page 15: "inparticular" changed to "in particular"

"supposing, that" changed to "supposing that"

Page 16: "393.4 mm" changed to "393.4 μμ"

Page 20: "for which stars if" changed to "for which stars it"

Page 22: "sphaerical" changed to "spherical"

Page 23: "principal scource" changed to "principal source"

Page 25: "lense with 15 cm" changed to "lens with 15 cm"

Page 27: "Through the spectroscopie method" changed to "Through the
spectroscopic method"

"made to its principal" changed to "made its principal"

"american manner" changed to "American manner"

Page 35: "many tenths of a year" changed to "many tens of years"

Page 38: "same appearence" changed to "same appearance"

Page 47: "red stears" changed to "red stars"

"_dispersion_ in M" changed to "_dispersion_ in _M_"

Page 49: "smaller the" changed to "smaller than"]

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