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Eddington Luminosity (L๐๐ฅ๐ฅ) โโ๏ฝDefinition๏ฝ1st๏ฝ20251119205401-00-โ
Eddington luminosity - Wikipedia
Eddington luminosity
The Eddington luminosity, also referred to as the Eddington limit, is the maximum luminosity a body (such as a star) can achieve when there is balance between the force of radiation acting outward and the gravitational force acting inward. The state of balance is called hydrostatic equilibrium. When a star exceeds the Eddington luminosity, it will initiate a very intense radiation-driven stellar wind from its outer layers. Since most massive stars have luminosities far below the Eddington luminosity, their winds are driven mostly by the less intense line absorption.1 The Eddington limit is invoked to explain the observed luminosities of accreting black holes such as quasars.
Originally, Sir Arthur Eddington took only the electron scattering into account when calculating this limit, something that now is called the classical Eddington limit. Nowadays, the modified Eddington limit also takes into account other radiation processes such as boundโfree and freeโfree radiation interaction.
Printed 2026-06-28.
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Link to original Footnotes
A. J. van Marle; S. P. Owocki; N. J. Shaviv (2008). โContinuum driven winds from super-Eddington stars. A tale of two limitsโ. AIP Conference Proceedings. 990: 250โ253. arXiv:0708.4207. Bibcode:2008AIPC..990..250V. doi:10.1063/1.2905555. S2CID 118364586. โฉ
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