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An Estimate of Solar Energetic Electrons from Polarization Observations of Millimeter Wave Emission

Research Project

Project/Area Number 61460008
Research Category

Grant-in-Aid for General Scientific Research (B)

Allocation TypeSingle-year Grants
Research Field Astronomy
Research InstitutionTokyo Astronomical Observatory, University of Tokyo

Principal Investigator

KAI Keizo  Tokyo Astronomical Observatory, University of Toky, Professor, 東京天文台, 教授 (70012846)

Co-Investigator(Kenkyū-buntansha) SEKIGUCHI Hideaki  Tokyo Astronomical Observatory, University of Tokyo, Technical staff, 東京天文台, 教務技官 (40154645)
SHIOMI Yasuhiko  Tokyo Astronomical Observatory, University of Tokyo, Assistant, 東京天文台, 助手 (00134627)
NAKAJIMA Hiroshi  Tokyo Astronomical Observatory, University of Tokyo, Lecturer (Iye,Masanori), 東京天文台, 講師 (40012877)
Project Period (FY) 1986 – 1987
Project Status Completed (Fiscal Year 1987)
Budget Amount *help
¥6,300,000 (Direct Cost: ¥6,300,000)
Fiscal Year 1987: ¥2,200,000 (Direct Cost: ¥2,200,000)
Fiscal Year 1986: ¥4,100,000 (Direct Cost: ¥4,100,000)
KeywordsSolar radio emission / High energy phenomena of the Sun / 偏波観測 / ミリ波電波 / 太陽高エネルギー電子 / ミリ波帯電波
Research Abstract

(1) Objective
We have proposed a new method for estimating energy spectra of nonthermal electrons prroduced in solar flares, using radio observations of bursts at mm wavelengths: the frequency (wavelengt h) dependence of both flux and polarization. The method can be used also for estimating the pol arity and intensity of magnetic fiels in the radio emitting region. These quantities could not otherwise be determined.
(2) Result
The frequency dependence of both flux and posarization was obtained for flare-associated bursts from observations made at three different frequencies with the 17, 35 and 80 GHz polarimeters at Nobeyama. Comparing the measured frequency dependence with that calculated based on gyrosynchrotron theory for various distribution functions of energetic electrons, we have obtained the following result: Hte energy spectrum of nonthermal electrons responsible for mmemission can be wxpressed as a power-law distribution. However it was found that the power-law distribution is not consistent with that independently derived from X-ray observations on the thick-target model, which has been widely accepeted as the X-ray emission model. How to resolve this discrepancy is a problem to be investigated in future.

Report

(2 results)
  • 1987 Final Research Report Summary
  • 1986 Annual Research Report
  • Research Products

    (8 results)

All Other

All Publications (8 results)

  • [Publications] 甲斐敬造: Solar Physics. 111. 81-87 (1987)

    • Description
      「研究成果報告書概要(和文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] 甲斐敬造: Solar Physics. (1988)

    • Description
      「研究成果報告書概要(和文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] 甲斐敬造: Solar Physics.

    • Description
      「研究成果報告書概要(和文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] K,Kai: "Microwave Sources of Solar flares: Loop Top or Foot Points ?" Solar Physics. 111. 81-87 (1987)

    • Description
      「研究成果報告書概要(欧文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] K,Kai: "Evidence for or against a Common Origin of Hard X-Rays and Microwaves from Solar Flares" Solar Physics. in press. (1988)

    • Description
      「研究成果報告書概要(欧文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] K.Kai: "Energy Spectra of Nonthermal Electrons of Solar Flares inferred from Hard X-Rays and Microwaves" Solar Physics. in preparation. (1988)

    • Description
      「研究成果報告書概要(欧文)」より
    • Related Report
      1987 Final Research Report Summary
  • [Publications] 甲斐敬造: Solar Physics. 104. 235-241 (1986)

    • Related Report
      1986 Annual Research Report
  • [Publications] 甲斐敬造: Solar Physics.

    • Related Report
      1986 Annual Research Report

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Published: 1987-03-31   Modified: 2016-04-21  

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