Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 44
... beta decay by the neutron - rich nuclei until stable or long - lived isobars are reached . Since the various reactions are subject to statistical fluctuations , a small spread in A develops at each mass for which ( n , y ) and ( y , n ) ...
... beta decay by the neutron - rich nuclei until stable or long - lived isobars are reached . Since the various reactions are subject to statistical fluctuations , a small spread in A develops at each mass for which ( n , y ) and ( y , n ) ...
Pagina 303
... beta - decay and also inverse beta - decay - the absorption of electrons from the Fermi sea . If the energy at the Fermi surface , Ep = mc2 [ ( 1 + x2 ) 1/2 - 1 ] , exceeds the energy for beta emission by the nucleus , ( Z — 1 , 4 ) ...
... beta - decay and also inverse beta - decay - the absorption of electrons from the Fermi sea . If the energy at the Fermi surface , Ep = mc2 [ ( 1 + x2 ) 1/2 - 1 ] , exceeds the energy for beta emission by the nucleus , ( Z — 1 , 4 ) ...
Pagina 304
... beta - decay , and must have a mass of 1.205 Mo , as compared with the maximum mass of 1.363 Mo , and associated central density of 109.499 for a pure Mg24 star . In fact , a magnesium star of this mass can achieve equi- librium near p ...
... beta - decay , and must have a mass of 1.205 Mo , as compared with the maximum mass of 1.363 Mo , and associated central density of 109.499 for a pure Mg24 star . In fact , a magnesium star of this mass can achieve equi- librium near p ...
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