Prospects for high-elevation radio detection of 0>10 PeV tau neutrinos
Prospects for high-elevation radio detection of 0>10 PeV tau neutrinos
复制标题
0>10 PeV tau 中微子高空射电探测前景
DOI：
10.1088/1475-7516/2020/11/065
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发表时间：
2020
影响因子：
6.4
通讯作者：
Ludwig, Andrew
中科院分区：
文献类型：
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作者：
Wissel, Stephanie;Romero-Wolf, Andrés;Schoorlemmer, Harm;Jr., Washington R.;Alvarez-Muñiz, Jaime;Zas, Enrique;Cummings, Austin;Deaconu, Cosmin;Hughes, Kaeli;Ludwig, Andrew
Tau中微子预计将包括大约三分之一的天体物理和宇宙成因的中微子通量，但目前的风味比约束不佳，预计在10 - 17 eV以上的能量通量低。我们提出了一个探测器的概念，旨在通过高海拔山顶探测器使用无线电技术测量在这个能量范围内的τ中微子的扩散通量。探测器搜寻由掠过地球的τ中微子产生的上行空气簇射的无线电信号。来自紧凑阵列中的几个天线的信号在触发电平上进行相干求和，不仅允许人为背景的定向掩蔽，而且允许低触发阈值。这种设计既利用了高海拔地区的大视野，又利用了无线电仪器几乎完整的占空比。我们目前的贸易研究，考虑站海拔，频带，阵列中的天线数量，和触发阈值，开发一个高效的站设计。这样的山顶探测器可以实现一个因素的100个独立的站在接受现有的仪器提高了10倍。通过1000个观测站和三年的观测，它可以实现对积分E− 2通量< 10− 9 GeV cm− 2 sr− 1 s− 1的灵敏度，在假设纯铁宇宙线组成的全味宇宙成因中微子的预期通量范围内。
Tau neutrinos are expected to comprise roughly one third of both the astrophysical and cosmogenic neutrino flux, but currently the flavor ratio is poorly constrained and the expected flux at energies above 10 17 eV is low. We present a detector concept aimed at measuring the diffuse flux of tau neutrinos in this energy range via a high-elevation mountaintop detector using the radio technique. The detector searches for radio signals from upgoing air showers generated by Earth-skimming tau neutrinos. Signals from several antennas in a compact array are coherently summed at the trigger level, permitting not only directional masking of anthropogenic backgrounds, but also a low trigger threshold. This design takes advantage of both the large viewing area available at high-elevation sites and the nearly full duty cycle available to radio instruments. We present trade studies that consider the station elevation, frequency band, number of antennas in the array, and the trigger threshold to develop a highly efficient station design. Such a mountaintop detector can achieve a factor of ten improvement in acceptance over existing instruments with 100 independent stations. With 1000 stations and three years of observation, it can achieve a sensitivity to an integrated Script E− 2 flux of< 10− 9 GeV cm− 2 sr− 1 s− 1, in the range of the expected flux of all-flavor cosmogenic neutrinos assuming a pure iron cosmic-ray composition.