Eddington limit

(ˈɛdɪŋtən)

(Astronomy) astronomy the theoretical upper limit of luminosity that a star of a given mass can reach; occurs when the outward force of the radiation just balances the inward gravitational force

[C20: named after A. S. Eddington (1882–1944), English astronomer and physicist]

Collins English Dictionary – Complete and Unabridged, 12th Edition 2014 © HarperCollins Publishers 1991, 1994, 1998, 2000, 2003, 2006, 2007, 2009, 2011, 2014

Translations

limite di Eddington

References in periodicals archive

which is the Eddington luminosity. Stars dominated by radiation pressure in their photosphere are fully determined by the photosphere, meaning that their luminosities will adjust to match the Eddington luminosity.

Physical properties of stars and stellar dynamics

(82-84) In this analysis, one needs to introduce the Eddington ratio [lambda], the bolometric luminosity divided by the Eddington luminosity, given as [L.sub.Edd] = 1.25 x [10.sup.38](M/M0) erg [s.sup.-1] for a black hole mass of M.

Cosmological evolution of supermassive black holes in galactic centers unveiled by hard X-ray observations

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