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 288
... Hoyle ( 1957 ) , and later in a more elaborate version Fowler and Hoyle ( 1960 , 1964 ) , have argued that the transition from iron to helium at a density of around 107 g / cm3 and a temperature of 7 × 109 ° K is sufficient to cause a ...
... Hoyle ( 1957 ) , and later in a more elaborate version Fowler and Hoyle ( 1960 , 1964 ) , have argued that the transition from iron to helium at a density of around 107 g / cm3 and a temperature of 7 × 109 ° K is sufficient to cause a ...
Pagina 322
... Hoyle ( 1960 ) , and later by Clayton ( 1964 ) . In order to avoid the necessity for an assumption of an explicit production distribution curve ( prompt , continuous , etc. ) , Fowler and Hoyle ( 1960 ) attempted to make use of the ...
... Hoyle ( 1960 ) , and later by Clayton ( 1964 ) . In order to avoid the necessity for an assumption of an explicit production distribution curve ( prompt , continuous , etc. ) , Fowler and Hoyle ( 1960 ) attempted to make use of the ...
Pagina 456
... Hoyle ( 1955 ) and later by Hoyle and Hazelgrove ( 1958 ) . There have been continual attempts to fit the observed color - magnitude diagrams to the theoretical color - magnitude diagrams for the globular clusters and for the galactic ...
... Hoyle ( 1955 ) and later by Hoyle and Hazelgrove ( 1958 ) . There have been continual attempts to fit the observed color - magnitude diagrams to the theoretical color - magnitude diagrams for the globular clusters and for the galactic ...
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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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