Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 24
... Cameron's abundances are listed in column 3 of Table 1 , and are plotted in Figure 2 when they differ from the SU values . Cameron's abundance table has been criticized by Burbidge ( 1960 , 1963 ) because of the many uncertainties which ...
... Cameron's abundances are listed in column 3 of Table 1 , and are plotted in Figure 2 when they differ from the SU values . Cameron's abundance table has been criticized by Burbidge ( 1960 , 1963 ) because of the many uncertainties which ...
Pagina 38
... Cameron's work ( Cameron 1959d , e ) the average neutron energy is 60 to 75 kev , while CFHZ and CF as- sume the relevant energy to be 25 kev . As mentioned above , Frank - Kamenet- skii uses 4.1 kev for the proper neutron energy . Only ...
... Cameron's work ( Cameron 1959d , e ) the average neutron energy is 60 to 75 kev , while CFHZ and CF as- sume the relevant energy to be 25 kev . As mentioned above , Frank - Kamenet- skii uses 4.1 kev for the proper neutron energy . Only ...
Pagina 332
... Cameron ( 1959 ) , the rate of production of He3 is very slow , and this might limit the number of explosions in 5 ... Cameron , other reactions that might also trigger nova explosions . Cameron considers the following reactions : 3He1 ...
... Cameron ( 1959 ) , the rate of production of He3 is very slow , and this might limit the number of explosions in 5 ... Cameron , other reactions that might also trigger nova explosions . Cameron considers the following reactions : 3He1 ...
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