Velocity-Dependent Eddington Factor in Relativistic Radiative Flow
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We propose a variable Eddington factor, depending on the flow velocity, v, for relativistic radiative flow, whose velocity becomes on the order of the speed of light. When the gaseous flow is radiatively accelerated up to the relativistic regime, the vclocity gradient becomes very large in the direction of the flow. As a result, the radiative diffusion may become anisotropic in the comoving frame of the gas. Hence, in a flow that is accelerated from subrelativjstic to relativistic regimes, the Eddington factor should be different from 1/3, even in the diffusion limit. As a simple form, the velocity-dependent Eddington factor may be written as f (Beta) =1/3 + (2/3)Beta, where Beta = v/c. Using the velocity-dependent Eddington factor, we can solve the rigorous equations of the relativistic radiative flow accelerated up to the relativistic speed. We also propose a generalized form for a variable Eddington factor as a function of the optical depth, tau, as well as the flow velocity, f(tau, Beta) = 1/3 + (2/3)[1 + (tau + 1)Beta]/(l + tau + Beta), for a spherically symmetric case. The velocity-dependent Eddington factor can be used in various relativistic radiatively-driven flows, such as black-hole accretion flows, relativistic astrophysical jets and outflows, and relativistic explosions like gamma-ray bursts.
収録刊行物
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- PASJ : publications of the Astronomical Society of Japan
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PASJ : publications of the Astronomical Society of Japan 58 461-467, 2006-04-25
Astronomical Society of Japan
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詳細情報 詳細情報について
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- CRID
- 1050564287757299456
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- NII論文ID
- 10023941077
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- NII書誌ID
- AA1082896X
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- ISSN
- 00046264
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- NDL書誌ID
- 7888037
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- 本文言語コード
- en
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- 資料種別
- journal article
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- データソース種別
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- IRDB
- NDL
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