multi-wavelength analysis of the impact polarization of 2001, june 15 th solar flare zhi xu (1),...
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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
The first Chinese-Korean Solar Physics Workshop 2005 July Beijing
Motion modeMotion mode& & velocity distribution velocity distribution functionfunction
NeutralizingElectrons(Return Current)
The first Chinese-Korean Solar Physics Workshop 2005 July Beijing
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
The first Chinese-Korean Solar Physics Workshop 2005 July Beijing
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 !
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