SOLAR FLARE OPTICAL SPECTROPOLARIMETRY

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Presentation transcript:

SOLAR FLARE OPTICAL SPECTROPOLARIMETRY Zhi XU (1,2), Jean-Claude HENOUX (1), Gilbert CHAMBE (1), Alexander PETRESHEN (3) and Cheng FANG (4) (1) OBSERVATOIRE DE PARIS, LESIA, France (2) YUNNAN OBSERVATORY, China (3) St PETERSBURG INSTITUTE OF OPTICS, Russia (4) NANJING UNIVERSITY, China Xu et al. 2005, ApJ, 631, 618 Xu et al. 2006, ApJ submitted 21/09/2018

THEMIS OBSERVATIONS June 15th 2001 Flare Hard X-rays X 65° HXRS 29 – 44 keV 44 – 67 keV 21/09/2018

2D distributions of Ha (left) and Hb (right) polarization (at 10:07 UT), and of the longitudinal magnetic field B//. P radial P tangential P radial 21/09/2018 Ha Hb

2D distribution of Ha, Hb and Mg I 552.84 nm line linear polarization at 10:07 UT Polarization: Radial: triangles Tangential: stars Ha (blue) Hb (green) Mg I (red) Line-center intensity contours Ha (dotted line) - - - - - MgI (solid line) 0.42 arc second square/pixel 21/09/2018

Time variation of Mg I line impact polarization 10 pixels averaged intensity (triangles) - polarization degree (stars) from 10:07 to 10:12 UT. 21/09/2018

CONCLUSIONS The Ha, Hb and Mg lines are linearly polarized. The highest polarization is observed at flare kernels borders. Radial linear polarization is present in Ha, Hb and Mg lines. Tangential linear polarization in Ha is also present . Both return current electrons associated with electron beams and low energy protons can explain the readial polarization observed. 21/09/2018