Stellar StructureUniversity of Chicago Press, 1965 - 648 pagine |
Dall'interno del libro
Risultati 1-3 di 87
Pagina 425
... observed to possess strong magnetic fields may , in fact , do so , and the actually observed fields may be underestimated . Again , a magnetic field like the sun's is far too weak to be observable in a distant star . It therefore seems ...
... observed to possess strong magnetic fields may , in fact , do so , and the actually observed fields may be underestimated . Again , a magnetic field like the sun's is far too weak to be observable in a distant star . It therefore seems ...
Pagina 458
... observed periods of magnetic stars unless the subsurface field is far greater than that observed at the surface . Also , in some torsional oscillations at least , it is possible for thin shells within the star to oscillate independently ...
... observed periods of magnetic stars unless the subsurface field is far greater than that observed at the surface . Also , in some torsional oscillations at least , it is possible for thin shells within the star to oscillate independently ...
Pagina 615
... observed HR diagrams are most frequently presented in terms of My and BV , the absolute visual magnitude and blue - visual color index of the UBV system ( Johnson and Morgan 1953 , Johnson and Harris 1954 , Johnson 1955 , 1963 ) . The ...
... observed HR diagrams are most frequently presented in terms of My and BV , the absolute visual magnitude and blue - visual color index of the UBV system ( Johnson and Morgan 1953 , Johnson and Harris 1954 , Johnson 1955 , 1963 ) . The ...
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