论文标题
木星中的wimp灭的单核中微子
Monoenergetic Neutrinos from WIMP Annihilation in Jupiter
论文作者
论文摘要
可以通过太阳捕获弱相互作用的巨大颗粒（WIMP）并在核心中歼灭，这可能会导致可在静止状态腐烂到单晶236 Mev中微子中的kaons产生。已经进行了对沙丘上中微子检测的几项研究。已经表明，如果WIMP质量低于4 GEV，那么它们将在歼灭之前蒸发，从而抑制信号。由于木星具有较冷的核心，因此在1-4 GEV范围内具有质量的wimps不会蒸发，因此可以将其歼灭成单位中微子。我们计算木星表面附近这些中微子的通量，发现它与在4 GEV高于4 GEV的沙丘上的通量相当，而在1-4 GEV范围内则更大。当然，检测这些中微子需要木星附近的中微子检测器。显然，要构建这样的检测器需要数十年的时间，但是应直接检测实验找到具有1-4 GEV范围内质量的WIMP，这可能是了解歼灭过程的几种方法之一。液体氢时间投影室可能能够获得这些中微子的精确方向信息和能量（氢在木星附近很丰富）。我们推测可以将这种检测器放在潮汐锁定的阿马尔斯卫星之一的远端。月球本身将提供大量的背景屏蔽，表面将使太阳能电池板更容易发电。
Weakly interacting massive particles (WIMPs) can be captured by the Sun and annihilate in the core, which may result in production of kaons that can decay at rest into monoenergetic 236 MeV neutrinos. Several studies of detection of these neutrinos at DUNE have been carried out. It has been shown that if the WIMP mass is below 4 GeV, then they will evaporate prior to annihilation, suppressing the signal. Since Jupiter has a cooler core, WIMPs with masses in the 1-4 GeV range will not evaporate and can thus annihilate into monoenergetic neutrinos. We calculate the flux of these neutrinos near the surface of Jupiter and find that it is comparable to the flux at DUNE for masses above 4 GeV and substantially greater in the 1-4 GeV range. Of course, detecting these neutrinos would require a neutrino detector near Jupiter. Obviously, it will be many decades before such a detector can be built, but should direct detection experiments find a WIMP with a mass in the 1-4 GeV range, it may be one of the few ways to learn about the annihilation process. A liquid hydrogen time projection chamber might be able to get precise directional information and energy of these neutrinos (and hydrogen is plentiful in the vicinity of Jupiter). We speculate that such a detector could be placed on the far side of one of the tidally locked Amalthean moons; the moon itself would provide substantial background shielding and the surface would allow easier deployment of solar panels for power generation.
