Development of a Method for Determining the Search Window for Solar Flare Neutrinos
Development of a Method for Determining the Search Window for Solar Flare Neutrinos
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DOI：
10.1007/s11207-020-01706-z
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发表时间：
2019-09
期刊：
影响因子：
2.8
通讯作者：
K. Okamoto;Y. Nakano;S. Masuda;Y. Itow;M. Miyake;T. Terasawa;S. Ito;M. Nakahata;M. Nakahata
中科院分区：
文献类型：
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作者：
K. Okamoto;Y. Nakano;S. Masuda;Y. Itow;M. Miyake;T. Terasawa;S. Ito;M. Nakahata;M. Nakahata
太阳耀斑期间产生的中微子仍然难以捉摸。然而，经过50年的讨论和搜索，他们的发现所释放的潜在知识使搜索变得至关重要。与太阳耀斑相关的中微子提供了关于太阳耀斑期间粒子加速机制的信息。对于中微子探测器来说，大气中微子和太阳耀斑中微子之间的分离在技术上受到能带重叠的阻碍。为了提高与背景中微子的区别，我们开发了一种方法来确定太阳耀斑期间中微子产生的时间搜索窗口。我们的方法是基于太阳卫星记录的数据，如地球静止运行环境卫星（GOES）、theReuven Ramaty高能太阳光谱成像仪（RHESSI）和GEOTAIL。在这项研究中，我们选择了1996年至2018年间发生的23次X5.0级以上的太阳耀斑。我们分析了中子捕获的软x射线、硬x射线、-射线、线射线的光曲线以及软x射线的导数。确定的平均搜索窗口如下：软x射线为4178 s，软x射线导数为700 s，硬x射线（100 - 800 keV）为944 s，中子捕获线射线为5 s，硬x射线（50 keV以上）为776 s。这种方法可以提高中微子探测器对太阳耀斑中微子的灵敏度。
Neutrinos generated during solar flares remain elusive. However, after 50 years of discussion and search, the potential knowledge unleashed by their discovery keeps the search crucial. Neutrinos associated with solar flares provide information on otherwise poorly known particle acceleration mechanisms during a solar flare. For neutrino detectors, the separation between atmospheric neutrinos and solar flare neutrinos is technically encumbered by an energy band overlap. To improve differentiation from background neutrinos, we developed a method to determine the temporal search window for neutrino production during solar flares. Our method is based on data recorded by solar satellites, such as theGeostationary Operational Environmental Satellite(GOES), theReuven Ramaty High Energy Solar Spectroscopic Imager(RHESSI), and GEOTAIL. In this study, we selected 23 solar flares above X5.0 class that occurred between 1996 and 2018. We analyzed the light curves of soft X-rays, hard X-rays,-rays, line-rays from neutron capture as well as the derivative of soft X-rays. The average search windows are determined as follows: 4178 s for soft X-ray, 700 s for the derivative of soft X-ray, 944 s for hard X-ray (100 – 800 keV),s for line-ray from neutron captures, and 776 s for hard X-ray (above 50 keV). This method allows neutrino detectors to improve their sensitivity to solar flare neutrinos.