Evolution

New PDF release: Stars and Stellar Evolution

By Klass S De Boer, W Seggewiss

ISBN-10: 2759803287

ISBN-13: 9782759803286

ISBN-10: 2759803562

ISBN-13: 9782759803569

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The gas pressure is Pgas = nkT . 37) with gas density ρ and gravitation according g = G M r 2 . 38) with κm = κm (T, P, XY Z) the temperature-, pressure-, composition-dependent mass absorption coeffiecient. This requires numerical solutions. 39) HP being the pressure scale height (equivalence height). The mean molecular weight, μ, for fully ionized gases is easy to calculate (Eq. 65) but for partially ionized gases (as is normally the case in stellar atmospheres) it is a complicated function of T, P, and XY Z.

The dwarfs established the main sequence (MS), the red giants the red-giant branch (RGB). Stars below the main sequence thus are “subdwarf (sd) stars”, stars on the lower part of the red giant branch are called “subgiants”, stars above the RGB “supergiants” (SGs). Later one discovered a strip of stars lying horizontally in the CMD, stars then called “horizontalbranch stars” (HB stars). 8 Summary The basic observational parameters of stellar astronomy are given: magnitudes, spectra, the Hertzsprung-Russell diagram, and further simple relations for the surface parameters of stars.

Two theoretical approaches are known in the literature. The collision theory considers the radiating atom when another particle passes close by. The wavetrain in the process of being emitted is disturbed and is now considered as a collection of small sections being emitted in time. The full line profile then follows from Fourier analysis. In the statistical approach one asks for which fraction of time is the spectral line shifted due to the influence of a colliding particle. The statistics leads then to the full profile.

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Stars and Stellar Evolution by Klass S De Boer, W Seggewiss


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