SEARCH FOR MUON POINT SOURCES BY USING THE OKAYAMA COUNTER TELESCOPE

到目前为止，关于从天鹅座X-3方向到达的μ子的几个谜题还没有得到解决。我们研制了一种新型的带磁谱仪的高原反望远镜，用于搜索介子点源。在望远镜中，人们可以跟踪一颗恒星，测量入射宇宙射线μ子的动量和电荷符号。望远镜由一个实心铁磁铁、三个定位室和两个伺服电机机构组成。望远镜位于冈山大学校园（北纬34 41′，东经133 55′）的海平面上。在每一天，天鹅座X-3（4.8小时周期）围绕目标穿过当地子午线的时刻被追踪5.5小时。跟踪天鹅座X-3的工作从1989年10月2日开始，现在仍在继续。我们报告了从天鹅座X-3方向到达的μ子的相位分析的初步结果。这些数据[周期：1989年10月2日- 1990年3月1日，入射角：<±>3.5平行于望远镜轴（即Cygn…更偏向于X-3方向）]被划分为动量区，分为mu^+和mu^-。在这个分析中，天鹅座X-3的周期是由van der Klis和Bonnet-Bidaud 1)得出的。动量区[4.0-22.5 GeV/c]的mu^-相图表明，在[0.65-0.70]相区间有4.7sigma的过剩，而该区域的mu^+和所有动量区域的mu^-总量均无过剩。在伽马射线观测2)和地下介子观测3)中已经报道了[0.6-0.7]的过量。然而，过去的实验不能表明在较低的动量[-10 GeV/c] mu^-处有过剩。这一点如果得到证实，将是一个全新的事实！到目前为止，假设μ子信号是真实的，可以推导出来自天鹅座X-3（被称为“小天鹅”）的母粒子的很强的约束条件。我们的结果需要任何修改约束，并使搜索其他父母成为可能。例如，我们可以考虑一个更小的动量nu_<mu>。加速器实验[nu mu (nu^^- mu) + N - mu^- (mu^+) +强子]5报道了观测到的介子角分布，峰值介子角为2‰，中微子总截面sigma nu^^-/sigma nu为- 1/3。这些结果与我们的结果并不矛盾。更重要的是，e可以振荡到但是^^-不是6)然而，在160 GeV以下的中微子总横截面为10^<-37> cm^2/核子^5)，因此必须有非常大的中微子通量[10^4 cm^<-2>sr^<-1>sec^<-1>]才能在这段时间内得到超过30 mu^-事件。结论是，我们的观测必须继续，mu^-过剩必须得到证实，这些观测结果导致了新的天鹅座X-3模型、中微子振荡实验和中微子望远镜。少

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