Astronomy:Von Zeipel theorem
In astrophysics, the von Zeipel theorem states that the radiative flux
The theorem is:
where the luminosity
This relation ignores the effect of convection in the envelope, so it primarily applies to early-type stars.[3]
According to the theory of rotating stars,[4] if the rotational velocity of a star depends only on the radius, it cannot simultaneously be in thermal and hydrostatic equilibrium. This is called the von Zeipel paradox. The paradox is resolved, however, if the rotational velocity also depends on height, or there is a meridional circulation. A similar situation may arise in accretion disks.[5]
References
- ↑ Zeipel, Edvard Hugo von (1924). "The radiative equilibrium of a rotating system of gaseous masses". Monthly Notices of the Royal Astronomical Society 84 (9): 665–719. doi:10.1093/mnras/84.9.665. Bibcode: 1924MNRAS..84..665V.
- ↑ Maeder, André (1999). "Stellar evolution with rotation IV: von Zeipel's theorem and anistropic losses of mass and angular momentum". Astronomy and Astrophysics 347: 185–193. Bibcode: 1999A&A...347..185M.
- ↑ Lucy, L. B. (1967). "Gravity-Darkening for Stars with Convective Envelopes". Zeitschrift für Astrophysik 65: 89. Bibcode: 1967ZA.....65...89L.
- ↑ Tassoul, J.-L. (1978). Theory of Rotating Stars. Princeton: Princeton Univ. Press.
- ↑ Kley, W.; Lin, D. N. C. (1998). "Two-Dimensional Viscous Accretion Disk Models. I. On Meridional Circulations In Radiative Regions". The Astrophysical Journal 397: 600–612. doi:10.1086/171818. Bibcode: 1992ApJ...397..600K.
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