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In astrophysics, the von Zeipel theorem states that the radiative flux F {\displaystyle F} in a uniformly rotating star is proportional to the local effective gravity g eff {\displaystyle g_{\text{eff}}}. The theorem is named after Swedish astronomer Edvard Hugo von Zeipel.
The theorem is:
where the luminosity L {\displaystyle L} and mass M ∗ {\displaystyle M_{*}} are evaluated on a surface of constant pressure P {\displaystyle P}. The effective temperature T eff {\displaystyle T_{\text{eff}}} can then be found at a given colatitude θ {\displaystyle \theta } from the local effective gravity:
This relation ignores the effect of convection in the envelope, so it primarily applies to early-type stars.