SEARCH FOR MUON POINT SOURCES BY USING THE OKAYAMA COUNTER TELESCOPE

使用冈山计数器望远镜搜索 μ 子点源

• 批准号: 62460016
• 负责人: WADA Tomonori
• 金额: $ 4.67万
• 依托单位: OKAYAMA UNIVERSITY
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (B)
• 财政年份: 1987
• 资助国家: 日本
• 起止时间: 1987 至 1989
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-62460016/
• 关键词: altazimuthal counter telescope; solid iron magnet; Cygnus X-3; follow up a star; phase analyses; muon point sources; 粒子望遠鏡; ミュ-オン点源探索; 点源追尾; 入射粒子運動量測定; ミューオン点源探索

Up to this time, several puzzles of arrival muons from the direction of Cygnus X-3 has not been solved. We have constructed a new altazimuthal counter telescope with a magnet spectrometer to search muon point sources. In the telescope, one can follow up a star and measure the momentum and the charge sign of incident cosmic-ray muons. The telescope consists of a solid iron magnet, three position chambers and two servo-motor mechanisms. The telescope is located at the campus of Okayama University (34ﾟ 41' N latitude, 133ﾟ 55' E longitude) at sea level. In each day, the Cygnus X-3 [4.8 hours period] is traced for 5.5 hours around a moment the target passed-through the local meridian. The tracing Cygnus X-3 have been operated from 02 October 1989 and now continue. We report preliminary results that are phase analyses of arrival muons from the Cygnus X-3 direction. The data [the period:02.10.1989 - 01.03.1990, incident angles:<plus-minus>3.5ﾟ parallel to the telescope axis (that is the Cygn … More us X-3 direction)] are classified into momentum regions and divided into mu^+ and mu^-. In this analysis, the period of Cygnus X-3 derived by van der Klis and Bonnet-Bidaud 1) was used. The phasegram of the mu^- in the momentum region [4.0-22.5 GeV/c] indicated a 4.7sigma excess in the [0.65-0.70] phase interval, and there are no excess in the mu^+ in the region and the total mu^- in all momentum regions. The excess in the [0.6-0.7] have been reported in gamma ray observations 2) and underground muons observations 3). However, past experiments could not indicate an excess at the lower momentum [-10 GeV/c] mu^-. This point is a completely new fact if confirmed! Until now, assuming that the muon signals were to turn to be genuine, very strong constrong constrains can be derived concerning the parent particle coming from Cygnus X-3, designated as "cygnet" 4). Our result demands any revised constrain and makes possible searching for other parents. For an example, one can consider a lower momentum nu_<mu> . The accelerator experiment [nu mu (nu^^- mu ) + N - mu^- (mu^+) + hadrons] 5) reported the observed distribution in muon angle, the peak muon angle was 2ﾟ and the neutrino total cross section sigma nu^^-/sigma nu was - 1/3. These results are not contradictory to our result. More, ne e can oscillate to nu mu but nu^^- not 6).However, the neutrino total cross section up to 160 GeV is 10^<-37> cm^2/nucleon^5), so it must be very large neutrino flux [10^4 cm^<-2>sr^<-1>sec^<-1>to get the excess of 30 mu^- events in this time.As the conclusion, our observations must be continued and the mu^- excess must be confirm, these observations lead a new Cygnus X-3 model, neutrino oscillation experiment and neutrino telescope. Less

到目前为止，天鹅座X-3方向的到达μ子的几个谜团还没有解决。我们已经建立了一个新的地平计数器望远镜与磁谱仪搜索μ介子点源。在望远镜中，人们可以跟踪一颗星星，测量入射宇宙射线μ子的动量和电荷符号。该望远镜由一个固体铁磁体、三个位置室和两个伺服电机机构组成。该望远镜位于冈山大学校园（北纬34 <$41 '，东经133 <$55'）的海平面上。每天，天鹅座X-3 [4.8小时周期]在目标通过当地子午线的瞬间被追踪5.5小时。追踪天鹅座X-3从1989年10月2日开始运行，现在仍在继续。我们报告的初步结果是从天鹅座X-3方向到达μ子的相位分析。数据[时间段：02.10.1989 - 01.03.1990，入射角：<plus-minus>3.5 °平行于望远镜轴（即天鹅座） ...更多信息 us X-3方向）]划分为动量区，并分为μ ^+和μ ^-。在这个分析中，使用了由货车·德·克利斯和邦纳-比多1）推导出的天鹅座X-3的周期。μ ^-在动量区[4.0-22.5 GeV/c]的相图表明，在[0.65-0.70]相区间有4.7 σ的过剩，而μ ^+在动量区和所有动量区的总μ ^-没有过剩。[0.6-0.7]中的过量已经在伽马射线观测2）和地下μ子观测3）中报道过。然而，过去的实验不能表明在较低的动量[-10 GeV/c] μ ^-下的过量。这是一个全新的事实，如果得到证实！到目前为止，假设μ子信号是真实的，可以导出关于来自天鹅座X-3的母粒子的非常强的共强约束，指定为“cygnet”4）。我们的结果要求任何修改的约束，并使可能寻找其他父母。例如，可以考虑较低的动量nu<mu>。加速器实验[nu mu（nu^^- mu）+N-mu ^-（mu^+）+强子] 5）报道了观测到的μ子角分布，μ子角峰值为2 μ，中微子总截面σ nu^^-/σ nu为-1/3。这些结果与我们的结果并不矛盾。然而，中微子总截面在160 GeV以下为10^<-37>cm ^2/核子^[5]，因此，要在这段时间内获得超过30 μ ^-事件，必须有很大的中微子通量[10 ^4 cm^<-2>sr^<-1>sec^]<-1>。因此，我们的观测必须继续下去，必须证实μ ^-事件的存在，这些观测结果将导致新的天鹅座X-3模型、中微子振荡实验和中微子望远镜的建立。少

项目成果

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Y.Yamashita,T.Wada,et al.: "Is Cygnus X-3 a Muon Point Source?" Proc.of 21st Int.Cosmic Ray Conf.

Y.Yamashita、T.Wada 等人：“Cygnus X-3 是 μ 子点源吗？”

H.Miyai,T.Wada,T.Katayama,M.Tsuruda,Y.Yamashita,I.Yamamoto and K.Saito:"A New Counter Telescope with a Magnet spectrometer" Proceedings of 21st International Cosmic Ray Conference,(Adelaide,Australia). 9. 429-432 (1990)

H.Miyai,T.Wada,T.Katayama,M.Tsuruda,Y.Yamashita,I.Yamamoto and K.Saito:“A New Counter Telescope with a Magnet Spectrometer”第21届国际宇宙射线会议论文集，（澳大利亚阿德莱德）

A.Benvenuti, et al.: Phys. Rev. Lett. 32.125-128, 1974.

A.Benvenuti 等人：物理学。

M. van der Klis and J.M.Boonet-Bidaud: Astro. Astrophys. 95. L5, 1981.

M. van der Klis 和 J.M.Boonet-Bidaud：Astro。