In astrophysics, the von Zeipel theorem states that the radiative flux ${\displaystyle F}$ in a uniformly rotating star is proportional to the local effective gravity ${\displaystyle g_{\text{eff))}$. The theorem is named after Swedish astronomer Edvard Hugo von Zeipel.

The theorem is:

${\displaystyle F=-{\frac {L(P)}{4\pi GM_{*}(P)))g_{\text{eff)),}$

where the luminosity ${\displaystyle L}$ and mass ${\displaystyle M_{*))$ are evaluated on a surface of constant pressure ${\displaystyle P}$. The effective temperature ${\displaystyle T_{\text{eff))}$ can then be found at a given colatitude ${\displaystyle \theta }$ from the local effective gravity:^[1][2]

${\displaystyle T_{\text{eff))(\theta )\sim g_{\text{eff))^{1/4}(\theta ).}$

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]