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
Risultati 1-3 di 15
Pagina 381
... PLANETARY NEBULA STAGE D. E. Osterbrock Planetary nebulae are very small gaseous emission nebulae that invariably have a hot blue star within them which emits ultraviolet radiation that ionizes and heats the gas . The nebulae are always ...
... PLANETARY NEBULA STAGE D. E. Osterbrock Planetary nebulae are very small gaseous emission nebulae that invariably have a hot blue star within them which emits ultraviolet radiation that ionizes and heats the gas . The nebulae are always ...
Pagina 382
... planetary ) , the angular size of shell in the sky is measured , and these two quantities give the distance to the planetary . If the apparent magnitude of the star in the planetary is then measured , its absolute magnitude becomes ...
... planetary ) , the angular size of shell in the sky is measured , and these two quantities give the distance to the planetary . If the apparent magnitude of the star in the planetary is then measured , its absolute magnitude becomes ...
Pagina 383
... planetary nebulae have ages of about 2.5 x 104 years . When they become even larger than this , they are too faint to discover , although presumably larger objects do exist , but are not found . In fact , the largest known planetary ...
... planetary nebulae have ages of about 2.5 x 104 years . When they become even larger than this , they are too faint to discover , although presumably larger objects do exist , but are not found . In fact , the largest known planetary ...
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 | |
30 sezioni non visualizzate
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