Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
Risultati 1-3 di 84
Pagina 61
... Fowler ( 1958 , 1959 ) , has been shown experimentally not to occur ( Bashkin , Kavanagh , and Parker 1959 ) . Reactions ( 3 ) and ( 4 ) proceed slowly at low temperatures . For ( 3 ) , the equilibrium ratio of He3 / H for stars ...
... Fowler ( 1958 , 1959 ) , has been shown experimentally not to occur ( Bashkin , Kavanagh , and Parker 1959 ) . Reactions ( 3 ) and ( 4 ) proceed slowly at low temperatures . For ( 3 ) , the equilibrium ratio of He3 / H for stars ...
Pagina 94
... Fowler and Hoyle ( 1960 ) , Kohman ( 1961 ) , and Fowler ( 1961 ) . The basis for this ap- proach consists of the assumptions that stellar formation has declined exponen- tially with time during the life of the Galaxy and that the ...
... Fowler and Hoyle ( 1960 ) , Kohman ( 1961 ) , and Fowler ( 1961 ) . The basis for this ap- proach consists of the assumptions that stellar formation has declined exponen- tially with time during the life of the Galaxy and that the ...
Pagina 185
... Fowler , Greenstein , and Hoyle 1962 ; Bashkin and Peaslee 1961 ) , while the re- actions C13 + He4 → 0 % + n , H1 + Ne 20 → Na21 + Y , Ne21 + He → Mg24 + n , Ne22 + He Mg25 + n , - > are expected to provide neutron fluxes for the ...
... Fowler , Greenstein , and Hoyle 1962 ; Bashkin and Peaslee 1961 ) , while the re- actions C13 + He4 → 0 % + n , H1 + Ne 20 → Na21 + Y , Ne21 + He → Mg24 + n , Ne22 + He Mg25 + n , - > are expected to provide neutron fluxes for the ...
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 atoms beta decay bound-free Burbidge calculations Cameron Chandrasekhar chemical composition clusters Coma Cluster computed considered constant conv convective zone core cross-section degeneracy density diagram discussed effect elements emission energy equation equilibrium evolutionary explosion formula Fowler fraction free-free galaxies Gaunt factors given gm/cm³ gravitational Greenstein He¹ He³ helium Hoyle HR diagram hydrogen hydrostatic equilibrium increase instability ionization isotopes km/sec layers light-curves lines of force luminosity magnetic field magnitude main sequence main-sequence mass maximum Mestel neutrino neutrons novae nuclear reactions nuclei observed obtained opacity oscillations particles perturbation photon Phys pressure radiation radiative radius ratio red giant region rotation s-process Sandage scattering Schatzman Schwarzschild sequence solar spectra spectrum star stellar evolution Strömgren supernovae of type surface Table temperature theory thermal tion velocity virial theorem white dwarf