Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 26
... elements . If , as assumed by HF , Type II supernovae are the source of the iron - group elements , with each supernova converting ten per cent of its mass into this portion of the abundance table , one such explosion per 400 years for ...
... elements . If , as assumed by HF , Type II supernovae are the source of the iron - group elements , with each supernova converting ten per cent of its mass into this portion of the abundance table , one such explosion per 400 years for ...
Pagina 55
... elements . On this basis , it is reasonable to assume that old galactic clusters have the same heavy - element content as young ones and that the Popu- lation II stars are richer in helium than expected on the evolutionary argument ...
... elements . On this basis , it is reasonable to assume that old galactic clusters have the same heavy - element content as young ones and that the Popu- lation II stars are richer in helium than expected on the evolutionary argument ...
Pagina 73
... elements in Apm stars . A revised discussion was given by Burbidge , Burbidge , and Fowler ( 1958 ) . Two alternatives were offered . In one , protons and alpha particles were flare - accelerated , thanks to the magnetic fields , to ...
... elements in Apm stars . A revised discussion was given by Burbidge , Burbidge , and Fowler ( 1958 ) . Two alternatives were offered . In one , protons and alpha particles were flare - accelerated , thanks to the magnetic fields , to ...
Sommario
Introduction | 1 |
Nuclear Abundances | 23 |
The Problem of the Nuclei of D He³ Li Be and | 60 |
Copyright | |
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absorption abundance approximation assumed astrophysical atoms BBFH beta decay bound-free Burbidge calculations Cameron Chandrasekhar clusters coefficients computed considered constant convective zone core cross-section decay degeneracy density diagram discussed effects elements emission energy equation equilibrium evolutionary flux formula Fowler fraction free electrons free-free galaxies Gaunt factors given globular clusters gm/cm³ gravitational Greenstein He¹ He³ helium Hoyle HR diagram hydrogen instability ionization ions isotopes Ledoux lines of force luminosity magnetic field magnitude main sequence main-sequence mass Mestel mixture neutrino neutrons novae nuclear reactions nuclei observed obtained opacity oscillations parameter particles perturbation photon Phys planetesimals pressure radiation radiative radius ratio red giant rotation s-process Sandage scattering Schwarzschild solar spectrum star stellar atmospheres stellar evolution stellar models Strömgren supernovae of type surface Table temperature theory thermal tion velocity virial theorem white dwarf