Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
Risultati 1-3 di 90
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 96
... Fowler ( 1961 ) then finds D = 7.7 X 109 years . Finally , 8 must be evaluated . This measures the average time it took the original stars to begin making r - elements . HF ( 1960 ) associated the r - process with stars of small mass ...
... Fowler ( 1961 ) then finds D = 7.7 X 109 years . Finally , 8 must be evaluated . This measures the average time it took the original stars to begin making r - elements . HF ( 1960 ) associated the r - process with stars of small mass ...
Pagina 185
... Fowler , Greenstein , and Hoyle 1962 ; Bashkin and Peaslee 1961 ) , while the re- actions C13 + He → 016 + n , H1 + Ne20 Na 21+ Y , Ne 21+ 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 + He → 016 + n , H1 + Ne20 Na 21+ Y , Ne 21+ He → Mg24 + n . Ne22 + He → Mg25 + n , are expected to provide neutron fluxes for 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