Von Zeipel theorem

The von Zeipel theorem in astrophysics states that the radiative flux, $F$, in a uniformly rotating star is proportional to the local effective gravity, $g\_\{eff\}$. Specifically,

$F=-frac\{L(P)\}\{4pi\; G\; M\_\{*\}(P)\}g\_\{eff\}$.

From this we can find the effective temperature, $T\_\{eff\}$, at a given colatitude, $heta$, from the local effective gravity

$T\_\{eff\}(\; heta)sim\; g\_\{eff\}^\{1/4\}(\; heta)$. [ cite journal
last = von Zeipel
first = H.
title = The radiative equilibrium of a rotating system of gaseous masses
journal = Mon. Not. R. Astron. Soc.
volume = 84
pages = 665–719
date = 1924] [ cite journal
last = Maeder
first = A.
title = Stellar evolution with rotation IV: von Zeipel's theorem and anistropic losses of mass and angular momentum
journal = Astronomy and Astrophysics
volume = 347
pages = 185-193
date = 1999]

References