Volume 42 Issue 1
Jan.  2022
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YANG Xiaohua, WANG Qixi, XIA Zhongfei, BAO Yun, PENG Dailiang, TIAN Tian, XU Long. Quantitative Characterization of Photospheric Magnetic Field in Solar Active Regions (in Chinese). Chinese Journal of Space Science,  2022, 42(1): 34-43.  DOI: 10.11728/cjss2022.01.200826076
Citation: YANG Xiaohua, WANG Qixi, XIA Zhongfei, BAO Yun, PENG Dailiang, TIAN Tian, XU Long. Quantitative Characterization of Photospheric Magnetic Field in Solar Active Regions (in Chinese). Chinese Journal of Space Science,  2022, 42(1): 34-43.  DOI: 10.11728/cjss2022.01.200826076

Quantitative Characterization of Photospheric Magnetic Field in Solar Active Regions

doi: 10.11728/cjss2022.01.200826076
  • Received Date: 2020-08-26
  • Accepted Date: 2020-08-26
  • Rev Recd Date: 2021-06-29
  • Available Online: 2022-05-25
  • In order to resolve the quantitative technique of photospheric magnetic field in solar active regions, all SOHO Michelson Doppler Interferometer (MDI) magnetograms from 1996 to 2011 have been used, and all solar active regions located within 45° solar surface angle have been segmented. The projection distortion of magnetogram area have been studied, then the consine factors for area correction have been established, and solar active regions area have been corrected. Based on the photospheric parameters quantified by Ref. [18–20], the index system has been built and improved, and it has been used to quantity characterization of magnetic field. The quantitative result has been analyzed by the Principal Component Analysis (PCA), and magnetic field of active region10486 erupted X17.2 flare has been analyzed. The results show that R, LPS, Lsg  and

    $\phi $

    PSL can explain the change of magnetic field structure in active region, and

    $\phi $

    uns,

    $\phi $

    ,

    $\phi $

    tot, and

    $\phi $

    mean can explain the change of magnetic flux in active region.

    $\phi $

    PSL is the new characteristic parameters in this paper. The above parameters can monitor the changes of magnetic field structure and magnetic flux in the active region effectively before and after the flare eruption; the quantitative results could be used as the input of flare, proton event monitoring and flare prediction model, and provided technical support for the monitoring and early warning of solar flare activity.

     

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