用兆吨级和千米^3探测器探测太阳中微子耀斑
Detecting Solar Neutrino Flare in Megaton and km^3 detectors
摘要：
为了预测太阳耀斑的中微子信号，我们推断了它的上下限。最近几年，人们根据观测到的太阳粒子耀斑，用一般的能量均分理论推导出了这个上限。根据2005年1月由太阳耀斑引起的硬γ碰撞的最新记录（中性π衰变），导出了中微子信号的最有说服力的下限，观测到的γ通量几乎是一对一地反映到中微子的相应γ通量中。因此，我们得到的最小界限已经在目前的边缘，但在不久的将来兆吨中微子探测器。这种探测器被认为主要是揭示宇宙超新星背景或罕见的本星系群（少数Mpc）超新星事件。然而，百万吨级甚至内部的十兆吨级冰立方探测器在十GeV的阈值下也可能揭示出太阳耀斑最硬能量中的太阳中微子痕迹。冰立方，也是。太阳中微子的味道可能会照亮中微子混合角。
英文摘要：
To foresee a solar flare neutrino signal we infer its upper and lower bound. The upper bound was derived since a few years by general energy equipartition arguments on observed solar particle flare. The lower bound, the most compelling one for any guarantee neutrino signal, is derived by most recent records of hard Gamma bump due to solar flare on January 2005 (by neutral pion decay).The observed gamma flux reflects into a corresponding one for the neutrinos, almost one to one. Therefore we obtain minimal bounds already at the edge of present but quite within near future Megaton neutrino detectors. Such detectors are considered mostly to reveal cosmic supernova background or rare Local Group (few Mpc) Supernovas events. However Megaton or even inner ten Megaton Ice Cube detector at ten GeV threshold may also reveal traces of solar neutrino in hardest energy of solar flares. Icecube, marginally, too. Solar neutrino flavors may shine light on neutrino mixing angles.
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。
