A Study of Neutral Particles from Cygnus X-3 above 10^<18>eV

10^<18>eV以上天鹅座X-3中性粒子的研究

• 批准号: 02452021
• 负责人: TESHIMA Masahiro
• 金额: $ 3.33万
• 依托单位: Institute for Cosmic Ray Research, University of Tokyo.
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (B)
• 财政年份: 1990
• 资助国家: 日本
• 起止时间: 1990 至 1991
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-02452021/
• 关键词: Cosmic Ray; Cygnus X-3; Gamma Ray; Neutral Particles; Air Shower; CygnusXー3; 空気シャワ-; 中性子; 高エネルギ-天文学; 宇宙線源

The Akeno Giant Air Shower Array (AGASA), covering 100km^2 area, has been in operation since 1990. This new array has accumulated more events than the number observed with the 20km^2 which has been in operation for over 5 years. Analysis of the data up through Nov 1991 to lood for excess in the direction of Cygnus X-3 shows 1 month that has a 4sigma excess number of events, occuring right after the strong radio burst of Jan 1991. No other time period shows a significant excess. The cummulative data set of AGASA shows a 2.5sigma excess in the direction of Cygnus X-3, still lower than necessary to make a strong claim for source emission. More data will be needed to clarify the characteristics of neutral emission from Cygnus X-3.We have improved the experiment in several ways to enhance sensitivity to neutral source emission. Installation of a detector calibration system gives us better rise time and gain certainty. The threshold energy of detectable showers has been decreased down to 10^<17>eV and the resulting trigger rate is lower (-0.1Hz). A new workstation in the central laboratory collects and writes the data to Magnetic Optical disks. These on-line systems are monitored and controlled from our Institute in Tokyo using telecommunications. Improvements have been made on analysis which have been used to measure the directional excess, test for periodicity, and search for bursts.

自1990年以来，Akeno巨型空气簇射阵列（AGASA）一直在运行，覆盖面积为100平方公里。这个新的阵列已经积累了比20 km^2观测到的更多的事件，20 km^2已经运行了5年多。对1991年11月至1999年11月期间天鹅座X-3方向的数据分析表明，在1991年1月的强射电爆发之后，有1个月的事件数量超过了4 σ。没有其他时间段显示出明显的过剩。AGASA的累积数据集显示天鹅座X-3方向有2.5 σ的过量，仍然低于强有力的源发射要求。天鹅座X-3的中性辐射特性还需要更多的数据来阐明。我们从几个方面改进了实验，以提高对中性源辐射的灵敏度。探测器校准系统的安装为我们提供了更好的上升时间和增益确定性。可探测簇射的阈值能量已经降低到10 μ <17>eV，并且由此产生的触发率更低（-0.1Hz）。中心实验室的一个新工作站收集数据并将其写入磁光盘。这些联机系统由我们在东京的研究所利用电信进行监测和控制。改进了用于测量方向性过剩、测试周期性和搜索爆发的分析方法。

项目成果

M.Nagano: "A New 100Km^2 Air Shower Array at Akeno(AGASA)" Astrophysical Aspects of The Most Energetic Cosmic Rays(Published by World Scientific). 335-344 (1991)

M.Nagano：“明野（AGASA）的新 100Km^2 空气淋浴阵列”最具能量宇宙射线的天体物理方面（由世界科学出版）。

M.Nagano: "A New 100km^2 Air Shower Array at Akeno(AGASA)" Astrophysical Aspects of The Most Energetic Cosmic Rays. (Published by World Scientific);. 335-344 (1991)

M.Nagano：“明野（AGASA）的新 100km^2 空气阵雨阵列”最具能量宇宙射线的天体物理方面。

S.Yoshida: "Propagation of the Highest Cosmic Rays I" Proc.21st ICRC(Adelaide). 3. 165-168 (1990)

S.Yoshida：“最高宇宙射线的传播 I”，红十字国际委员会第 21 届会议（阿德莱德）。

N.Hayashida et al.: "A Search for Point Sources above 10^<17>eV using Data from the Akeno Giant Air Shower Array" Proc.of 22nd International Cosmic Ray Conference (Dublin). Vol.1. 309-312 (1991)

N.Hayashida等人：“使用来自Akeno巨型空气簇射阵列的数据搜索10^ 17 eV以上的点源”第22届国际宇宙射线会议（都柏林）的会议记录。

N.Hayashida et al.: "A Search for Point Sources above 10^<17>eV using Data from the Akeno Giant Air Shower Array" Proc.of 22nd International Cosmic Ray Conference(Dublin). 1. 309-312 (1991)

N.Hayashida等人：“使用来自Akeno巨型空气簇射阵列的数据搜索10^ 17 eV以上的点源”第22届国际宇宙射线会议（都柏林）的会议记录。