SYNOPSIS OF A COURSE OF LECTURES
By PROFESSOR H. N. RUSSELL
At the University of Toronto during February, 1924
Two or more lectures will be devoted to each division
- I. The Extent of the Universe.
- Distances and Motions of the Stars. Motion of the Sun. Its use for measuring greater distances. The Brightness of the Stars. Apparent and Absolute Magnitudes. Star Colors and their measurement. Variable Stars, and their use in determining great distances. Distances of Star Clusters and the Milky W.ay.
- II. The Sizes and Masses of the Stars.
- Stellar Diameters. Eclipsing Variables. Interferometer measures. Stellar Masses. Binary Stars. Slow-moving pairs. Relation of mass to brightness. Similarity of Masses. Dynamical Parallaxes. Stellar Densities. Giant and Dwarf Stars.
- III. The Analysis of Light.
- The Observation of Spectra. The Origin of Spectra. Modern Atomic Theory. Excitation and Ionization of Atoms. The Interpretation of Complex Spectra. Black Body Radiation.
- IV. The Analysis of Stellar Atmospheres.
- The Sequence of Stellar Spectra-s-its dependence on Temperature. Temperatures found from color-index or heat-index. Stellar Diameters. The effects of Density. Spectroscopic Parallaxes. Saha's Theory of Ionization. -Pressure in Stars. Electron haze. Problem of the Photosphere.
- V. The Constitution and Evolution of the Stars.
- The Interior of a Star. Radiation Pressure. Eddington's Theory. What determines Stellar masses. Relation between Stars and Atoms. Stellar Evolution. Giant and Dwarf Stars. Influence of mass. The B-stars. The Time Scale. Age of the Earth and Sun. Probable origin of the Solar System. Sources of Stellar Energy. Special problems. Cepheid variables. Long-period variables. Novae.
- VI. The Nebulae.
- Dark Nebulae-their abundance, size and probable nature. Galactic Nebulae-gaseous and otherwise. Appearance. Spectra. Relation to Stars. Source of Luminosity. Probable Nature. Non-galactic Nebulae-Spiral and globular Forms. Spectra. Motions. Probable size and distance. Jeans's theory of their nature
|Russell Lecture, Feb 1924 (PDF)||1.59 MB|