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    Lectures on Stellar Statistics
    Lectures on Stellar Statistics
    Lectures on Stellar Statistics
    Ebook110 pages1 hour

    Lectures on Stellar Statistics

    By C. V. L. Charlier

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    "Lectures on Stellar Statistics" by C. V. L. Charlier. Published by Good Press. Good Press publishes a wide range of titles that encompasses every genre. From well-known classics & literary fiction and non-fiction to forgotten−or yet undiscovered gems−of world literature, we issue the books that need to be read. Each Good Press edition has been meticulously edited and formatted to boost readability for all e-readers and devices. Our goal is to produce eBooks that are user-friendly and accessible to everyone in a high-quality digital format.
    LanguageEnglish
    PublisherGood Press
    Release dateDec 2, 2019
    ISBN4057664598707
    Lectures on Stellar Statistics

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      Book preview

      Lectures on Stellar Statistics - C. V. L. Charlier

      C. V. L. Charlier

      Lectures on Stellar Statistics

      Published by Good Press, 2022

      [email protected]

      EAN 4057664598707

      Table of Contents

      CHAPTER I. APPARENT ATTRIBUTES OF THE STARS.

      1.

      2.

      3.

      4.

      5.

      6.

      7.

      8.

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      10.

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      14.

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      CHAPTER II. SOURCES OF OUR PRESENT KNOWLEDGE OF THE STARS.

      18.

      19.

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      22.

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      24.

      25.

      26.

      27.

      28.

      CHAPTER III. SOME GROUPS OF KNOWN STARS.

      29.

      30.

      31.

      32.

      33.

      34.

      CHAPTER I.

      APPARENT ATTRIBUTES OF THE STARS.

      Table of Contents

      1.

      Table of Contents

      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 place:—

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

      (2) the mean wave-length (λ0) 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.

      Table of Contents

      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) = (174435),

      so that the last two figures are in 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 attributes.

      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 lectures.

      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)

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