REHEATING AFTER INFLATION
REHEATING AFTER INFLATION
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DOI：
10.1103/physrevlett.73.3195
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发表时间：
1994-12-12
影响因子：
8.6
通讯作者：
STAROBINSKY, AA
中科院分区：
文献类型：
--
作者：
KOFMAN, L;LINDE, A;STAROBINSKY, AA
膨胀后宇宙重新加热的理论得到发展。我们发现，通常在重新加热的第一阶段，由于广泛的参数共振，经典暴胀场 迅速衰减为 粒子或其他玻色子。然后这些玻色子衰变成其他粒子，最终被热化。只有在单个粒子 φ 可以衰变成其他粒子的理论中，完全再加热才有可能。这对暴胀模型的结构施加了严格的限制，并意味着暴胀场可以是暗物质的候选者。
The theory of reheating of the Universe after inflation is developed. We have found that typically at the first stage of reheating the classical inflation field φ rapidly decays into φ particles or into other bosons due to a broad parametric resonance. Then these bosons decay into other particles, which eventually become thermalized. Complete reheating is possible only in those theories where a single particle φ can decay into other particles. This imposes strong constraints on the structure of inflationary models, and implies that the inflation field can be a dark matter candidate.