Pregalactic black hole accretion and the thermal history of the Universe
Pregalactic black hole accretion and the thermal history of the Universe
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DOI：
10.1093/mnras/194.3.639
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发表时间：
1981-03
影响因子：
4.8
通讯作者：
B. Carr
中科院分区：
文献类型：
--
作者：
B. Carr
银河系前的黑洞在早期可能因为吸积而有很大的光度。质量超过103 <$− 1 M <$（其中<$是辐射“效率”因子）的黑洞在退耦后一定会在爱丁顿极限下辐射一段时间，而足够大的黑洞可能会一直辐射到星系形成。由此产生的辐射可能对宇宙的热历史产生重要影响，即使黑洞的密度很小。一般来说，物质的温度会被提高到弗里德曼值以上，并且对于很宽的空穴质量和密度值，物质会完全再电离。在某些情况下，宇宙永远不会经历中性阶段。可以想象，在退耦之前的黑洞吸积可能产生了3 K背景辐射，但前提是黑洞的光度超过了爱丁顿极限。
Pregalactic black holes could have a large luminosity at early times due to accretion. Holes with mass exceeding about 103∊−1M⊙(where∊is the radiative ‘efficiency’ factor) would necessarily radiate at the Eddington limit for some period after decoupling, and large enough holes might do so until galaxy formation. The consequent radiation production could have an important effect on the thermal history of the Universe, even if the density of the holes is small. In general the matter temperature would be boosted well above its Friedmann value and, for a wide range ot values for the mass and density of the holes, the matter would be completely re-ionized. In some circumstances, the Universe would never pass through a neutral phase at all. Black hole accretionbeforedecoupling may conceivably have generated the 3 K background radiation, but only if the holes’ luminosity exceeded the Eddington limit.