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gravity darkening exponent

نمای ِ تاریکش ِ گرانشی

nemâ-ye târikeš-e gerâneši

Fr.: exposant de l'assombrissement gravitationnel

The exponent appearing in the power law that describes the
→ effective temperature of a → rotating star
as a function of the → effective gravity, as deduced from the
→ von Zeipel theorem or law. Generalizing this law, the effective
temperature is usually expressed as
T_{eff}∝ g_{eff}^{β}, where
β is the gravity darkening exponent with a value of 0.25. It has, however, been shown that
the relation between the effective temperature and gravity is not exactly a power law. Moreover,
the value of β = 0.25 is appropriate only in the limit of slow rotators and is
smaller for fast rotating stars (Espinosa Lara & Rieutord, 2011, A&A 533, A43).