论文标题
致密中微子气味的风味发展的新发展
New Developments in Flavor Evolution of a Dense Neutrino Gas
论文作者
论文摘要
中微子 - 中微子折射占主导地位的核心偏离超新星，中子星级合并和早期宇宙的风味。普通的中微子风味转化在由真空振荡频率确定的时间尺度上发展。但是，当中微子密度足够大时，由于成对中微子散射，可能会出现集体风味转换。成对转化率被认为是快速的，因为预计会发生在依赖中微子 - 中微子相互作用能量（即中微子数量密度）上的时间尺度上，并且受电子中微子和抗雷替氏菌的角度分布进行调节。快速成对转换的神秘现象已经忽略了很长时间。但是，由于快速转化率，成对转换可能发生在中微子去耦区域的接近性中，并且尚未理解对天体物理源的流体动力学和重元素的合成。我们回顾了这种引人入胜的现象的物理学及其对中微子致密来源的影响。
Neutrino-neutrino refraction dominates the flavor evolution in core-collapse supernovae, neutron-star mergers, and the early universe. Ordinary neutrino flavor conversion develops on timescales determined by the vacuum oscillation frequency. However, when the neutrino density is large enough, collective flavor conversion may arise because of pairwise neutrino scattering. Pairwise conversion is deemed to be fast as it is expected to occur on timescales that depend on the neutrino-neutrino interaction energy (i.e., on the neutrino number density) and is regulated by the angular distributions of electron neutrinos and antineutrinos. The enigmatic phenomenon of fast pairwise conversion has been overlooked for a long time. However, because of the fast conversion rate, pairwise conversion may possibly occur in the proximity of the neutrino decoupling region with yet to be understood implications for the hydrodynamics of astrophysical sources and the synthesis of the heavy elements. We review the physics of this fascinating phenomenon and its implications for neutrino-dense sources.
