Английская Википедия:Hubble–Reynolds law
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The Hubble–Reynolds law models the surface brightness of elliptical galaxies as
- <math>I(R) = \frac{I_0}{(1+R/R_H)^2}</math>
Where <math>I(R)</math> is the surface brightness at radius <math>R</math>, <math>I_0</math> is the central brightness, and <math>R_H</math> is the radius at which the surface brightness is diminished by a factor of 1/4. It is asymptotically similar to the De Vaucouleurs' law which is a special case of the Sersic profile for elliptical galaxies.[1]
The law is named for the astronomers Edwin Hubble and John Henry Reynolds. It was first formulated by Reynolds in 1913[2] from his observations of galaxies (then still known as nebulae). It was later re-derived by Hubble in 1930[3] specifically in observations of elliptical galaxies.
References
- ↑ Binney & Tremaine. Galactic Dynamics 2008.
- ↑ Шаблон:Cite journal
- ↑ Шаблон:Cite journal
