Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan.

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Presentation transcript:

Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan Observatory of Chinese Academy of Sciences (2) Observatoire de Paris, LESIA, France (3) Nanjing Unverisity, China The first Chinese-Korean Solar Physics Workshop 2005 July Beijing

X 65° THEMIS (French-Italian solar telescope) Flare Spectropolarimetric Observations Start Time The first Chinese-Korean Solar Physics Workshop 2005 July Beijing associated with hard X-ray and radio flux impulsive emissions … 10:07UT :30 UT I +S and I -S spectra of : Ha, Hb, FeI, Na I D1, D2

Linear Polarization Analysis Alignment of I+S and I-S signals Intensity gradient The first Chinese-Korean Solar Physics Workshop 2005 July Beijing Polarization degree: Polarization direction: Orientation reference axis of THEMIS, defining the Q and U Stokes parameters

Spatial distribution of the polarization degree and orientation Transverse field (Fe I) Longitudinal field (Fe I) perpendicular parallel (tangential) (radial) The first Chinese-Korean Solar Physics Workshop 2005 July Beijing

Ha Hb 10:07:2010:08:5410:13:3810:15:1310:10:29 Time dependence --- Intensity, polarization degree, orientation 4% in Ha and 6% in Hb line center in the early phase. Three main association of Ha and Hb polarization direction.

The first Chinese-Korean Solar Physics Workshop 2005 July Beijing LINEAR POLARIZATION of the H  line: Red: Protons Green: Electrons H  IMPACT POLARIZATION ENERGY DEPENDENCE

Electrons (E>E 0 ) or protons (E E 0 ) or protons (E<E 0 ) moving along the local solar magnetic field B p e Line of Sight Solar Disk Solar Surface Electrons (E>E 0 ) or protons (E<E 0 ) circling around the local solar magnetic field Solar Disk B p e Line of Sight Solar Surface The first Chinese-Korean Solar Physics Workshop 2005 July Beijing Motion mode & velocity distribution function

Neutralizing Electrons (Return Current) The first Chinese-Korean Solar Physics Workshop 2005 July Beijing Electron Beam Proton Beam tangential or radialradial Diagnostic for return current electrons

all local electrons Return Current carried by runaway electrons The first Chinese-Korean Solar Physics Workshop 2005 July Beijing

The Ha, Hb  lines are linearly polarized. The Ha, Hb  lines are linearly polarized. The highest polarization is observed around the brightest part of the flare kernels. The highest polarization is observed around the brightest part of the flare kernels. The directions are either parallel or perpendicular to the local transverse magnetic field. The directions are either parallel or perpendicular to the local transverse magnetic field. Jointed observations with RHESSI are needed. Firstova, Xu and Fang ( 2003, ApJ, 595L 131.) The first Chinese-Korean Solar Physics Workshop 2005 July Beijing CONCLUSIONS + hard X-ray + radio flux + center-reversal Ha intensity profiles … High energy particle beams bombard the chromosphere Bombardment by low energy protons or by high energy electrons associated with return currents can explain the polarization observed in Ha and Hb lines. ( no hard X-ray or microwave emission hect keV protons )

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