Stellar Evolution: Proceedings of an International Conference, November 13-15, 1963Robert F. Stein, Alastair Graham Walter Cameron Plenum Press, 1966 - 464 pagine |
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Pagina 194
... Curve ( 2 ) corresponds to the equal flux condition which depends on the value of ß . Curve ( 1 ) corresponds to the onset of convective instability , that is , ( n + 1 ) adiabatic ( n + 1 ) radiative In the region of the temperature ...
... Curve ( 2 ) corresponds to the equal flux condition which depends on the value of ß . Curve ( 1 ) corresponds to the onset of convective instability , that is , ( n + 1 ) adiabatic ( n + 1 ) radiative In the region of the temperature ...
Pagina 196
... Curve a is the calculated surface condition . Curve c shows the effect of neglecting the hydrogen - molecule dissociation zone . Curve b shows the effect of increasing the constant of opacity by 2.5 . For L 10-2Lo , the effect of ...
... Curve a is the calculated surface condition . Curve c shows the effect of neglecting the hydrogen - molecule dissociation zone . Curve b shows the effect of increasing the constant of opacity by 2.5 . For L 10-2Lo , the effect of ...
Pagina 408
... curve of the unknown object . The energy curves shown in Figures 1 to 3 were obtained in this way , using the extremely hot star BD + 28 ° 4211 as the standard . Having available the energy curves , let us now consider the nature of the ...
... curve of the unknown object . The energy curves shown in Figures 1 to 3 were obtained in this way , using the extremely hot star BD + 28 ° 4211 as the standard . Having available the energy curves , let us now consider the nature of the ...
Sommario
Nuclear Energy Generation in Stars and Some Aspects of Nucleosynthesis | 83 |
Radiative Absorption and Opacity Calculations | 123 |
Energy Transport by Turbulent Convection | 143 |
Copyright | |
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Parole e frasi comuni
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