Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 269
Stanley Bashkin Lawrence Hugh Aller, Dean Benjamin McLaughlin. Stellar Models for Main - Sequence Stars and Subdwarfs BENGT STRÖMGREN Institute for Advanced Study , Princeton , New Jersey ... Main-Sequence Stars with Masses Larger than 1 7 ...
Stanley Bashkin Lawrence Hugh Aller, Dean Benjamin McLaughlin. Stellar Models for Main - Sequence Stars and Subdwarfs BENGT STRÖMGREN Institute for Advanced Study , Princeton , New Jersey ... Main-Sequence Stars with Masses Larger than 1 7 ...
Pagina 320
... main sequence to evolve into the giant region are of mass near 1.15 Mo. Stars slightly more massive will have passed ... main sequence . The argument is not circular , even though it depends on age estimates derived by considering just ...
... main sequence to evolve into the giant region are of mass near 1.15 Mo. Stars slightly more massive will have passed ... main sequence . The argument is not circular , even though it depends on age estimates derived by considering just ...
Pagina 585
... main - sequence stage for stars of 28 Mo and higher ( corresponding to Mbol < -5 ) is about 30000 ° K , according to the computations of Schwarzschild and Härm . They did not compare their tracks with observations ... Main-Sequence Stages.
... main - sequence stage for stars of 28 Mo and higher ( corresponding to Mbol < -5 ) is about 30000 ° K , according to the computations of Schwarzschild and Härm . They did not compare their tracks with observations ... Main-Sequence Stages.
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