Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 369
... magnitude interval 2 Novae in the Milky Way -5 -3 -2 -1 1 2 3 5 visual magnitude FIG . 1. - Distribution in apparent visual magnitudes m , of the brightest known novae which appeared during the last 700 years and for which reliable data ...
... magnitude interval 2 Novae in the Milky Way -5 -3 -2 -1 1 2 3 5 visual magnitude FIG . 1. - Distribution in apparent visual magnitudes m , of the brightest known novae which appeared during the last 700 years and for which reliable data ...
Pagina 388
... magnitude interval dm is , of course , the smaller , relative to dN , the fainter the supernovae are , since images of these supernovae appear above the limiting magnitude my of a given search for ever shorter intervals 7 of time ...
... magnitude interval dm is , of course , the smaller , relative to dN , the fainter the supernovae are , since images of these supernovae appear above the limiting magnitude my of a given search for ever shorter intervals 7 of time ...
Pagina 460
... magnitude , though rather less in HD 188041 than in most of the rest . Thus the discrepancy in periods is difficult to explain if the period depends on the same physical properties as the magnitude of the field . Little more than this ...
... magnitude , though rather less in HD 188041 than in most of the rest . Thus the discrepancy in periods is difficult to explain if the period depends on the same physical properties as the magnitude of the field . Little more than this ...
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