Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
Risultati 1-3 di 98
Pagina 262
... Table 3 and others are indicated to show how linear interpolation in the hydrogen weight fraction , X , can give opacities to better than about 5 per cent accuracy with tables spaced as far apart as 0.6 in X. § 6. USE OF OPACITIES 6.1 ...
... Table 3 and others are indicated to show how linear interpolation in the hydrogen weight fraction , X , can give opacities to better than about 5 per cent accuracy with tables spaced as far apart as 0.6 in X. § 6. USE OF OPACITIES 6.1 ...
Pagina 275
... Table 1 with the observational material just referred to suggests that the choice of X values 0.60 and 0.70 and Z values 0.02 , 0.03 , and 0.04 provides composi- tion ranges that are adequate for Population I stars . In fact , the ...
... Table 1 with the observational material just referred to suggests that the choice of X values 0.60 and 0.70 and Z values 0.02 , 0.03 , and 0.04 provides composi- tion ranges that are adequate for Population I stars . In fact , the ...
Pagina 616
... Table 2 ) , with a well - determined parallax of 0.104 ( Wyller 1955 ) . The absolute visual magnitude is My = +2.98 , from the apparent magnitude ( Johnson and Morgan 1953 ) , corrected for the light of the secondary ( van den Bos 1959 ) ...
... Table 2 ) , with a well - determined parallax of 0.104 ( Wyller 1955 ) . The absolute visual magnitude is My = +2.98 , from the apparent magnitude ( Johnson and Morgan 1953 ) , corrected for the light of the secondary ( van den Bos 1959 ) ...
Sommario
THE ORIGIN OF THE CHEMICAL ELEMENTS | 1 |
The Age of Astronomical Objects | 87 |
References | 98 |
Copyright | |
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absorption abundance approximation assumed atoms BBFH beta decay bound-free Burbidge calculations Cameron CFHZ Chandrasekhar chemical composition clusters CNO cycle computed considered constant conv convective zone core cross-section decay density discussed effects electron elements emission energy equation equilibrium evolutionary factor flux Fowler galactic galaxies given globular clusters gm/cm³ gravitational Greenstein He¹ He³ helium Hoyle HR diagram hydrogen Ibid instability ionization isotopes layers Ledoux lines of force luminosity magnetic field magnitude main sequence main-sequence mass Mestel neutrino neutrons novae nuclear reactions nuclei observed obtained opacity oscillations particles perturbation Phys planetesimals pressure protons radiation radiative radius ratio red giant region rotation s-process Sandage Schwarzschild solar spectra spectrum stability star stellar evolution stellar models Strömgren supernovae of type surface Table temperature theory thermal tion turbulent variations velocity virial theorem white dwarf