Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 588
... Schwarzschild ( SES , p . 228 ; Schwarzschild and Härm 1962 ) . = An alternate possibility is that , after the helium flash has removed the de- generacy , the stellar model retains an inhomogeneous structure consisting of a helium ...
... Schwarzschild ( SES , p . 228 ; Schwarzschild and Härm 1962 ) . = An alternate possibility is that , after the helium flash has removed the de- generacy , the stellar model retains an inhomogeneous structure consisting of a helium ...
Pagina 589
... Schwarzschild ( 1952 ) were applied by them to the globular - cluster stars . But as was shown by Hoyle and Schwarz- schild degeneracy and convective envelopes needed to be taken into account . These corrections are not so important for ...
... Schwarzschild ( 1952 ) were applied by them to the globular - cluster stars . But as was shown by Hoyle and Schwarz- schild degeneracy and convective envelopes needed to be taken into account . These corrections are not so important for ...
Pagina 622
... Schwarzschild ( 1955 ) followed essentially the pro- cedure of Sandage and Schwarzschild ( 1952 ) , except that they integrated over the change in luminosity from the initial model to an advanced model ( beyond which , they noted , the ...
... Schwarzschild ( 1955 ) followed essentially the pro- cedure of Sandage and Schwarzschild ( 1952 ) , except that they integrated over the change in luminosity from the initial model to an advanced model ( beyond which , they noted , the ...
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