Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
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Pagina 484
... variations in μ below the level at which they sensibly affect the structure . The time of travel from core to ... variations over a sphere resulting from horizontal μ - variations △ μ / μ to generate " μ - current " velocities " of ...
... variations in μ below the level at which they sensibly affect the structure . The time of travel from core to ... variations over a sphere resulting from horizontal μ - variations △ μ / μ to generate " μ - current " velocities " of ...
Pagina 486
... variation of the 0 - average of μ ( r , 0 ) is absorbed into a 。( r ) . The energy equation ( 3.4 ) then yields for ... variations in T , and slow μ - currents ; rather one has to think in terms of a near discontinuity in μ , continuity ...
... variation of the 0 - average of μ ( r , 0 ) is absorbed into a 。( r ) . The energy equation ( 3.4 ) then yields for ... variations in T , and slow μ - currents ; rather one has to think in terms of a near discontinuity in μ , continuity ...
Pagina 503
... variations denoted by a prime are taken locally , and all spatial operators are invariant . In the second , the variations denoted by d are taken following the motion , and the spatial operators are not invariant . When more than one ...
... variations denoted by a prime are taken locally , and all spatial operators are invariant . In the second , the variations denoted by d are taken following the motion , and the spatial operators are not invariant . When more than one ...
Sommario
THE ORIGIN OF THE CHEMICAL ELEMENTS | 1 |
The Age of Astronomical Objects | 87 |
References | 98 |
Copyright | |
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absorption abundance approximation assumed atoms BBFH beta decay bound-free Burbidge calculations Cameron CFHZ Chandrasekhar chemical composition clusters CNO cycle computed considered constant conv convective zone core cross-section decay density discussed effects electron elements emission energy equation equilibrium evolutionary factor flux Fowler galactic galaxies given globular clusters gm/cm³ gravitational Greenstein He¹ He³ helium Hoyle HR diagram hydrogen Ibid instability ionization isotopes layers Ledoux lines of force luminosity magnetic field magnitude main sequence main-sequence mass Mestel neutrino neutrons novae nuclear reactions nuclei observed obtained opacity oscillations particles perturbation Phys planetesimals pressure protons radiation radiative radius ratio red giant region rotation s-process Sandage Schwarzschild solar spectra spectrum stability star stellar evolution stellar models Strömgren supernovae of type surface Table temperature theory thermal tion turbulent variations velocity virial theorem white dwarf