我们能测量宇宙中微子背景吗？
Can one measure the Cosmic Neutrino Background?
摘要：
宇宙微波背景（CMB）提供了大爆炸（BB）后约38万年的宇宙信息。由于中微子与物质的弱相互作用，宇宙中微子背景（CNB）应该提供有关我们宇宙更早时间的信息，大约在大爆炸后一秒。也许最有希望的方法来“看到”宇宙中微子背景是捕获电子中微子从背景的氚，然后衰变成3 He和一个电子的能量的Q值= 18.562 keV加上电子中微子静止质量。正在筹备中的“卡尔斯鲁厄氚中微子”实验似乎是目前提出的测量电子反中微子质量的最灵敏的方法。同时KATRIN还可以通过反应来寻找：电子中微子（~1.95开尔文）+3 H--> 3 He + e-（能量Q = 18.6 keV +电子中微子质量）。宇宙背景中微子（CNB）的捕获在电子谱中应表现为一个由电子中微子静止质量大于Q的峰。这里的可能性看到的CNB与KATRIN研究。KATRIN目前似乎不可能检测到CNB。但是KATRIN应该能够确定CNB局部电子中微子密度的上限。
英文摘要：
The Cosmic Microwave Background (CMB) yields information about our Universe at around 380 000 years after the Big Bang (BB). Due to the weak interaction of the neutrinos with matter the Cosmic Neutrino Background (CNB) should give information about a much earlier time of our Universe, around one second after the Big Bang. Probably the most promising method to `see' the Cosmic Neutrino Background is the capture of the electron neutrinos from the Background by Tritium, which then decays into 3He and an electron with the energy of the the Q-value = 18.562 keV plus the electron neutrino rest mass. The `KArlsruhe TRItium Neutrino' (KATRIN) experiment, which is in preparation, seems presently the most sensitive proposed method for measuring the electron antineutrino mass. At the same time KATRIN can also look by the reaction: electron neutrino (~1.95 Kelvin) + 3H --> 3He + e- (with the energy Q = 18.6 keV + electron neutrino mass). The capture of the Cosmic Background Neutrinos (CNB) should show in the electron spectrum as a peak by the electron neutrino rest mass above Q. Here the possibility to see the CNB with KATRIN is studied. A detection of the CNB by KATRIN seems not to be possible at the moment. But KATRIN should be able to determine an upper limit for the local electron neutrino density of the CNB.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
