Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 22
... abundance ratio is presumably related to such nuclear developments as the carbon cycle . However , Bidelman ( 1961 ) has found that variations in the relative abundance of the carbon isotopes in some carbon stars deficient in hydrogen ...
... abundance ratio is presumably related to such nuclear developments as the carbon cycle . However , Bidelman ( 1961 ) has found that variations in the relative abundance of the carbon isotopes in some carbon stars deficient in hydrogen ...
Pagina 24
... abundances of the other Zr isotopes are fixed using the SU isotope ratios . 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 ...
... abundances of the other Zr isotopes are fixed using the SU isotope ratios . 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 ...
Pagina 70
... abundance of 1 in chondrites , so the sun now appears overabundant in Be relative to chondrites . With Shima's lithium abundance , it appears that the solar Li / Be ratio is 1/700 that of mete- oritic matter ; previously this ratio was ...
... abundance of 1 in chondrites , so the sun now appears overabundant in Be relative to chondrites . With Shima's lithium abundance , it appears that the solar Li / Be ratio is 1/700 that of mete- oritic matter ; previously this ratio was ...
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