Proceedings of the International School of Physics "Enrico Fermi.", Volume 28N. Zanichelli, 1963 - Nuclear physics |
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Page 361
... adiabatic gradient Vad ( since in an exactly adiabatic layer no energy can be transported by adiabatically changing elements ) . Therefore we have V , >> ▽ ad • Now we assume with E. VITENSE ( 1953 ) that the rising hot elements will ...
... adiabatic gradient Vad ( since in an exactly adiabatic layer no energy can be transported by adiabatically changing elements ) . Therefore we have V , >> ▽ ad • Now we assume with E. VITENSE ( 1953 ) that the rising hot elements will ...
Page 374
... adiabatic theory . - 31. The quasi - adiabatic approximation . Although the pulsational energy is strictly conserved in the adiabatic theory , we may use the adiabatic ap- proximation in order to make a first estimate of the radiative ...
... adiabatic theory . - 31. The quasi - adiabatic approximation . Although the pulsational energy is strictly conserved in the adiabatic theory , we may use the adiabatic ap- proximation in order to make a first estimate of the radiative ...
Page 378
... adiabatic region , which contributes neither to the damp- ing nor driving as long as we are considering only radiative mechanisms . Hence our attention is centered on the intermediate nonadiabatic region , which usually produces a ...
... adiabatic region , which contributes neither to the damp- ing nor driving as long as we are considering only radiative mechanisms . Hence our attention is centered on the intermediate nonadiabatic region , which usually produces a ...
Contents
GRATTON Stellar evolution Introductory lecture | 1 |
A R SANDAGE and L GRATTON | 12 |
G BURBIDGE Nuclear astrophysics | 174 |
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absorption abundance adiabatic angular momentum assume B2FH BURBIDGE calculations CAMERON Cepheids chemical composition close binary components computed consider constant contraction convective zone core corresponding cosmic-ray decreases density derive discussion effect ejected electrons elements emission lines energy equation equilibrium evolutionary tracks factor flare stars flux FOWLER function g/cm³ galactic galaxies given globular clusters gradient gravitational H-R diagram helium HOYLE hydrogen increase instability interstellar ionization isotopes km/s layer LEDOUX light curves luminosity magnetic field magnitude main sequence massive stars motion nebula nebular variables neutrinos neutron nuclei O-associations observed obtain opacity particles phase Phys problem protons pulsation r-process radiation radiative radius ratio region relation rotation SALPETER SANDAGE SCHWARZSCHILD solar spectral type spectrum stellar associations stellar evolution subdwarfs subgiant supernova surface Tauri stars temperature theory thermal velocity white dwarfs