Composition of Heavy Elements in Solar Fiare Particles Associated with <gamma>-rays and Neutron Emission
| Project/Area Number |
61460013
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| Research Category |
Grant-in-Aid for General Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Research Field |
核・宇宙線・素粒子
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| Research Institution | Ibaraki University |
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Principal Investigator |
YANAGITE Shohei Department of Earth Sciences, Ibaraki University, 理学部, 助教授 (40013429)
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| Co-Investigator(Kenkyū-buntansha) |
近藤 一郎 東京大学, 宇宙線研究所, 教授 (80022523)
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| Project Period (FY) |
1986 – 1987
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| Project Status |
Completed (Fiscal Year 1987)
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| Budget Amount *help |
¥8,700,000 (Direct Cost: ¥8,700,000)
Fiscal Year 1987: ¥500,000 (Direct Cost: ¥500,000)
Fiscal Year 1986: ¥8,200,000 (Direct Cost: ¥8,200,000)
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| Keywords | Cosmic Rays / Solar Flare / Heavy Nuclei / γ-rays and Neutron / 太陽フレア / フレア粒子 / 元素組成 / ガンマ線 / 中性子 / 宇宙線の起源 |
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| Research Abstract |
The purpose of this project is to investigate the abundance of heavy elements in solar flare Particles associated with-<gamma>-ray and neutron emission which characterizes high energy nuclear reactions occurred at the flare site. The observation has been made The University of Chicago cosmic ray telescope on the ISEE-3 spacecraft. Our data were obtained from 1978 through 1982. The way of our analysis id the<DELTA>E-E method ehich utilizes two silicon detectors (D1 and D3) as <DELTA>E counter, and one CsI scintillator (D4) ad E counter. Before using this method, we must determine the conversion factor form pulse height to energy for each detector. We develope and establish a new calibration method which utilizes fully the power of two Cerenkov counters with a Cerenkov theshold [[5 and [[1.58 for each. The silicon silicon detectors were calibrated by comparison of the pulse height in each detector with the calculated eneregy deposit of minimum ionizing heavy ions which are selected by the signal from the Cerenkov counters. After setablishing the calibration of the silicon detectors, we can calibrate the CsI by relying on the tracks of each elements on D1(or D3) vs D4 scatter plot. Thus methoddoes not require linear response from D4. the energy spectrum of He have been analyzed for 1982 June 3 flare which exhibits emission of <gamma>rays from <pi>^゜decay and neutrons. Near future, will be determined the abundance of heavy elements including Li, Be, B which shows the evidence for high energy nuclear reactions in peculiar solar flares.
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Report
(2 results)
Research Products
(6 results)
