Stellar Evolution: Proceedings of an International Conference, November 13-15, 1963Robert F. Stein, Alastair Graham Walter Cameron Plenum Press, 1966 - 464 pagine |
Dall'interno del libro
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Pagina 151
... instability . It amounted to asking whether the buoyancy force on a displaced parcel of fluid is restorative or not . Actually , the instability criterion derived in this way is not a sufficient condition . For not only must the ...
... instability . It amounted to asking whether the buoyancy force on a displaced parcel of fluid is restorative or not . Actually , the instability criterion derived in this way is not a sufficient condition . For not only must the ...
Pagina 333
... INSTABILITY Norman Baker INTRODUCTION Of the various approaches which have been used to study stellar pulsation , the technique which in recent years has received the most attention is the stability analysis of the linearized equations ...
... INSTABILITY Norman Baker INTRODUCTION Of the various approaches which have been used to study stellar pulsation , the technique which in recent years has received the most attention is the stability analysis of the linearized equations ...
Pagina 357
... instability strip in approximately the right location , stability when insufficient helium is present , etc. ) , the instabilities found here are very likely of an actual physical origin and not merely a reflection of spurious ...
... instability strip in approximately the right location , stability when insufficient helium is present , etc. ) , the instabilities found here are very likely of an actual physical origin and not merely a reflection of spurious ...
Sommario
Nuclear Energy Generation in Stars and Some Aspects of Nucleosynthesis | 83 |
Radiative Absorption and Opacity Calculations | 123 |
Energy Transport by Turbulent Convection | 143 |
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absorption abundance adiabatic amplitude approximation assumed Astron Astrophys Bahcall C¹² calculations carbon carbon-burning central density central temperature Chiu composition condition constant convective zone core curve decrease degenerate determined effective temperature electron energy envelope equation evolutionary track factor fluctuation interactions fully convective function g/cm³ galactic galaxy H-R diagram Hayashi He³ heat helium flash helium-burning Hertzsprung-Russell diagram Hoyle hydrogen hydrogen-burning hydrostatic equilibrium increases initial interstellar interstellar medium ionization isotopes layer lines lithium luminosity main sequence main-sequence mass fraction mass loss massive stars modes neutrino neutrino processes neutrons nuclear burning nuclear reactions nuclei observed obtained opacity oxygen parameter phase photon photosphere Phys planetary population I stars population II pressure pulsation R₁ radiation radiative radius ratio region Schwarzschild shell source shown in Figure solar stage stellar evolution stellar structure supernova surface Table Tauri stars theory tion turbulence unstable velocity white dwarf