Effective temperature

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The articles Star Surface # Surface Temperature and Effective Temperature thematically overlap. Help me to better differentiate or merge the articles (→  instructions ) . To do this, take part in the relevant redundancy discussion . Please remove this module only after the redundancy has been completely processed and do not forget to include the relevant entry on the redundancy discussion page{{ Done | 1 = ~~~~}}to mark. McBayne ( discussion ) 10:21 p.m. , Jun 23, 2018 (CEST)

Spectral radiation density of our sun (effective temperature around 5780  K ) compared to that of a black body of the same size (labeling in English)

The effective temperature of a star is the temperature of its surface that a black body would have to have in order to shine with the same brightness per area . The effective temperature of an object deviates from the kinetically defined temperature, the less the spectrum of the object corresponds to that of a black body.

According to the Stefan-Boltzmann law, the following applies

with the Stefan-Boltzmann constant

This gives the bolometric brightness to


  • the star's surface , where is the radius of the star.

Since the stellar radius cannot be clearly defined, the optical density is used to calculate the effective temperature .

The effective temperature and the bolometric brightness are the two physical parameters with which a star can be classified in the Hertzsprung-Russell diagram .