Multi-wavelength analysis of the Multi-wavelength analysis of the impact polarization impact polarization

of 2001, June 15of 2001, June 15thth solar flare 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 --- 10:30 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 signalsIntensity gradient

The first Chinese-Korean Solar Physics Workshop 2005 July Beijing

Polarization degree:

Polarization direction:

I

QUP

22

)arctan(2

1

Q

U

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

The first Chinese-Korean Solar Physics Workshop 2005 July Beijing

Ha

Hb

10:07:20 10:08:54 10:13:38 10:15:1310:10:29

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

thE

0E

),90( 0 EPLINEAR POLARIZATION of the H line:

Red: Protons

Green: Electrons

HH IMPACT POLARIZATION IMPACT POLARIZATION ENERGY DEPENDENCE ENERGY DEPENDENCE

Electrons (E>EElectrons (E>E00) ) or or protons (E<Eprotons (E<E00)) moving almoving along the local solar magnetic fieldong the local solar magnetic field

Bp

eLine of Sight

Solar Disk Solar Surface

Electrons (E>E0) or protons (E<E0) circling around the local solar magnetic field

Solar Disk B

p

eLine of Sight

Solar Surface

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Motion modeMotion mode& & velocity distribution velocity distribution functionfunction

NeutralizingElectrons(Return Current)

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Electron Beam Proton Beam

tangential or radial radial

Diagnostic for return current electrons

0nJ

eRe nn ee

Re nC- expnn

ee

R nC expn

V

all local electrons

Return Current carried by

runaway electrons

e

R

nV

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The Ha, HbThe Ha, Hb lines are linearlylines are linearly polarizedpolarized.. The highest polarization is observed around the brighThe highest polarization is observed around the brightest part of the flare kernels.test part of the flare kernels. The directions are either parallel or perpendicular to tThe directions are either parallel or perpendicular to the local transverse magnetic field.he 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

CONCLUSIONSCONCLUSIONS

+ 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 microwa

ve emission hect keV protons )

감사하십시요 !