Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 450
... turbulence , so the slow decay due to finite conductivity can be supplemented by a much larger decay due to turbulence . The effect is , roughly , that turbulent motion may split the field into much smaller elements , whose smaller size ...
... turbulence , so the slow decay due to finite conductivity can be supplemented by a much larger decay due to turbulence . The effect is , roughly , that turbulent motion may split the field into much smaller elements , whose smaller size ...
Pagina 493
... turbulent energy transport is negligible , so that radiative equilibrium under superadiabatic tem- perature gradients is the correct zero - order approximation . On the main se- quence the subphotospheric convection zone goes over from ...
... turbulent energy transport is negligible , so that radiative equilibrium under superadiabatic tem- perature gradients is the correct zero - order approximation . On the main se- quence the subphotospheric convection zone goes over from ...
Pagina 508
... turbulent , as seems to be the case in the earth's atmos- phere . Then the coefficient of molecular and radiative viscosity in equation ( 2.26 ) should be replaced by the appropriate value for turbulent viscosity , which may be 1010 ...
... turbulent , as seems to be the case in the earth's atmos- phere . Then the coefficient of molecular and radiative viscosity in equation ( 2.26 ) should be replaced by the appropriate value for turbulent viscosity , which may be 1010 ...
Sommario
Introduction | 1 |
Nuclear Abundances | 23 |
The Problem of the Nuclei of D He³ Li Be and | 60 |
Copyright | |
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absorption abundance approximation assumed astrophysical atoms BBFH beta decay bound-free Burbidge calculations Cameron Chandrasekhar clusters coefficients computed considered constant convective zone core cross-section decay degeneracy density diagram discussed effects elements emission energy equation equilibrium evolutionary flux formula Fowler fraction free electrons free-free galaxies Gaunt factors given globular clusters gm/cm³ gravitational Greenstein He¹ He³ helium Hoyle HR diagram hydrogen instability ionization ions isotopes Ledoux lines of force luminosity magnetic field magnitude main sequence main-sequence mass Mestel mixture neutrino neutrons novae nuclear reactions nuclei observed obtained opacity oscillations parameter particles perturbation photon Phys planetesimals pressure radiation radiative radius ratio red giant rotation s-process Sandage scattering Schwarzschild solar spectrum star stellar atmospheres stellar evolution stellar models Strömgren supernovae of type surface Table temperature theory thermal tion velocity virial theorem white dwarf