The von Zeipel theorem in astrophysics establishes a relationship between the nuclear brightness of a point on the surface of a rotating star and the local effective acceleration. Qualitatively, due to rotation and oblateness, the equator of a rotating star is less bright than its poles.[1] References 1. ^ von Zeipel, H. (1924). "The radiative equilibrium of a rotating system of gaseous masses". Mon. Not. R. Astron. Soc. 84: 665-719.
Retrieved from "http://en.wikipedia.org/"
|
|
