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Nonlinear force-free Nonlinear force-free coronal magnetic field coronal magnetic field extrapolation scheme extrapolation scheme
for solar active regionsfor solar active regions
Han He, Huaning Wang, Yihua YanHan He, Huaning Wang, Yihua YanNational Astronomical Observatories, Chinese AcadeNational Astronomical Observatories, Chinese Acade
my of Sciences, Beijing, Chinamy of Sciences, Beijing, China
Hinode WorkshopHinode WorkshopBeijing, ChinaBeijing, China
Dec. 8-10, 2007Dec. 8-10, 2007
Solar eruption events are Solar eruption events are connected with the coronal connected with the coronal
magnetic structuresmagnetic structures
Direct observation Calculation based on a physical modelOR
Nonlinear force-free field Nonlinear force-free field (NLFFF) extrapolation for solar (NLFFF) extrapolation for solar
active regionsactive regions
vector magnetogram observed in the phot
osphere
magnetic field configuration in
the corona
Calculation based on
NLFFF model
?iB
Solar active region x
yz
Given Bx, By, Bz at the bottom boundary
BrB )(
0 B)(~ BJ
field line
B
JB //
0)( BB orForce-free:
Divergence-free:
The field can be considered force-free roughly 400km (0.55 arc second) above the photosphere(Metcalf et al., 1995, ApJ, 439, 474)
0 BAlpha is a constant along one field line
Nonlinear force-free field Nonlinear force-free field (NLFFF) model(NLFFF) model
Direct Boundary Integral Equation Direct Boundary Integral Equation (DBIE) method for NLFFF (DBIE) method for NLFFF extrapolationextrapolation((Yan, Y., Li, Z. 2006, ApJ, Yan, Y., Li, Z. 2006, ApJ, 638638, 1162, 1162))
x
y
z
0BB :
:0 B
BB
)( 2 rOB
dd 00 BBBz
Y
n
Yi
0d)( 22 BBB Y
)( ir
4
)cos(
4
)cos(),(Y
irr irr
Infinite plane surface boundary
),,( iii zyx
),,( iii zyx
),,( zyx
n
Boundary condition of DBIE Boundary condition of DBIE methodmethod
Infinite plane surface boundary
d0BBz
Yi
)( 2 rOB
vector magnetogram
B is assumed to be zero out of the vector magnetogram
Parameter Parameter λλ► same dimension as the force-free fsame dimension as the force-free f
actor actor αα►defined locally at a field pointdefined locally at a field point
► three components three components λλxx, , λλyy, , λλz z correspocorrespo
nding to Bnding to Bxx, B, Byy, B, Bzz
4
)cos(
4
)cos(),(Y
Optimal method to determine Optimal method to determine λλ and B locall and B locallyy((Yan, Y., Li, Z. 2006, ApJ, Yan, Y., Li, Z. 2006, ApJ, 638638, 1162, 1162))
d0BBn
Yi
0BB :
),,( zyxii BB
),,( find ***zyx
||||
||),,(
BJ
BJzyxif
),,(min),,( ***zyxizyxi ff
),,( iii zyx
Best convergence property at the field points near the bottom Best convergence property at the field points near the bottom boundaryboundary
•The bottom boundary for applying the DBIE is moved upwardly layer by layer to achieve the best convergence property
•Enlarge the area for integration at higher layers•Keep the original number of pixels at each layer to save computing time
Upward boundary integration Upward boundary integration schemescheme
0Layer 1Layer
2Layer 3Layer
4Layer
5Layer
region active
Output region of the code
0B
Global field configuration
Test Case ITest Case I► Low and Lou (1990) analytical fieldLow and Lou (1990) analytical field► 4/,3.0,1,1 lmn
xz
Case I 3D-ViewCase I 3D-View
Analytical solution
Extrapolated field
TestTest Case IICase II5/4,3.0,1,3 lmn
Global field configuration
►
x
z
Case II 3D-ViewCase II 3D-View
Analytical solution
Extrapolated field
The degree of agreement between the extrapolated field and the analytical solution
2/122
vec
i iii
iii bBbBC
The extrapolated fields deviate from the analytical fields gradually with the increase in height
)a(
)d()c(
)b(height vsfLheight vsfL
height vsdL height vsdL
I Case
solution analytical field edextrapolat
solution analytical field edextrapolat
I CaseI Case
I Case
Internal consistency of the extrapolated Field Internal consistency of the extrapolated Field (Case I)(Case I)
Vf VBV
L d)(1 22 BB
vd V
VL d
1 2B
Force-free and divergence-free constraints are satisfied in the extrapolated field
)a(
)d()c(
)b(height vsfLheight vsfL
height vsdL height vsdL
II Case
solution analytical field edextrapolat
solution analytical field edextrapolat
II CaseII Case
II Case
Internal consistency of the extrapolated Field Internal consistency of the extrapolated Field (Case II)(Case II)
Force-free and divergence-free constraints are satisfied in the extrapolated field
NLFFF extrapolation for solar active NLFFF extrapolation for solar active regionregion
NOAA 9077NOAA 9077
2000.07.14 04:14UT
Vector magnetogram of NOAA 9077 was observed at 04:14 UT on 14 July 2000 bySolar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station (HSOS)
Bx By Bz0
Bx By Bz1
The noises in the boundary data can be suppressed by DBIE through the integration over the whole boundary
AR 90772000.7.1404:14UT
Observed by SMFT at Huairou
FOV: 269x269 arcsec
64x64 grid4.2 arcsec/pixel~ 3000km/pixel
Red: field lines that leave Red: field lines that leave the modeling boxthe modeling box
Blue: closed field linesBlue: closed field lines
NS
(b)
(c) (d)
c
(a)
Internal consistency of the extrapolated field
height vsfL 9077NOAA height vsdL 9077NOAA
Vf VBV
L d)(1 22 BB
vd VV
L d1 2
B
Force-free constraint Divergence-free constraint
U-shaped field lines above the X-U-shaped field lines above the X-pointpoint
Side view
3D view
Compared with filament Compared with filament imagesimages
04:27UTTop view 04:14UT
(HSOS) filtergram H
04:12UT
TRACE 195A
Compared with TRACE imagesCompared with TRACE images
Before the flare During the flare (http://trace.lmsal.com)
maximum10:10UT
Onset of the flare
04:14UT
10:24UT
SOHO MDINOAA 10436 2003.08.22Vector magnetogram was observed at
2003.08.22 01:29:57UT bySolar Flare Telescope
NLFFF extrapolation for solar active NLFFF extrapolation for solar active regionregion
NOAA 10436NOAA 10436
AR 104362003.8.2201:29:57UT
Solar Flare Telescope
Lower layersLower layers
Red: field lines that leave the modeling boxRed: field lines that leave the modeling box Blue: closed field linesBlue: closed field lines
Compared with coronal imageCompared with coronal image NOAA 10436 NOAA 10436
GOES 12 SXI2003.08.2201:30:37UT
Solar Flare Telescope2003.08.22 01:29:57UT340 x 320 arcsec
64 x 64 grid5.3 arcsec/pixel
HHinode (Solar-B)inode (Solar-B)
SOT
XRT
EIS
Field of View
EIS (576”x512”)
XRT(2048”x2048”)
SOT:NFI/SP(328”x164”)SOT: BFI
(205”x102”)
N
E W
S
(From Hinode Team)
The instruments
46.8” X 162.3” (156 X 512 grids) 46.8” X 162.3” (156 X 512 grids)
Hinode Solar Optical Telescope – Spectro-polarimeterHinode Solar Optical Telescope – Spectro-polarimeter
Fast Map:Time per position: 3.2 sec
162.3” x 0.3”
Normal map
Fast map
Dynamics
Deep magnetogram
Sample dataSample data2007-6-4 08:49:04 - 08:58:54UT2007-6-4 08:49:04 - 08:58:54UT
Hinode Solar Optical Telescope (SOT)Hinode Solar Optical Telescope (SOT)Spectro-PolarimeterSpectro-Polarimeter (SP)(SP)-- -- level-0 datalevel-0 data
Level-0 dataLevel-0 data
I Q U V
Spectral coverage: 630.08nm - 630.32nm Fe I lines 630.15 and 630.25 nm
Hinode SOT SP level-1Hinode SOT SP level-1 data (by SSW code)data (by SSW code)
Level-1 dataLevel-1 dataI Q U V
Milne-Eddington inversion code (High Altitude ObservatorMilne-Eddington inversion code (High Altitude Observatory)y)
I Q
U V
NLFFF extrapolation for solar active NLFFF extrapolation for solar active regionregion
NOAA 10930NOAA 10930► Flare event: 2006.12.13 Flare event: 2006.12.13 0214 0240 0257UT X3.40214 0240 0257UT X3.4
SOHO MDINOAA 10930 2006.12.12
Vector magnetogram was observed at20:30UT on 12 Dec. 2006 by Hinode satellite
Images of Images of Hinode SOT Hinode SOT Spectro-Polarimeter Spectro-Polarimeter NOAA 10930 (630.15 nm)NOAA 10930 (630.15 nm)
I
Time of the observation :2006.12.12 20:30-21:33UT
FOV : 295.20 x 162.30 arcsecOriginal grid number : 1000 x 512
Q
U V
Level-1 dataLevel-1 data
Remove 180 degree ambiguity of the Remove 180 degree ambiguity of the direction of the transverse field direction of the transverse field
componentcomponent
By a reference field with a force-free factor best fitting the observed fields Wang, Yan and Sakurai (2001)
Vector magnetogram of NOAA 1093Vector magnetogram of NOAA 10930 0 Hinode SOT SP data
Time : 2006.12.12 20:30-21:33UTFOV : 295.20 x 162.30 arcsec
Original grid number : 1000 x 512Grid number for extrapolation : 111 x 60 (2.7arcsec/pixel)
Milne-Eddington inversion code by High Altitude ObservatoryMilne-Eddington inversion code by High Altitude Observatory
Compared with coronal image observed by Compared with coronal image observed by XRTXRT
NOAA 10930NOAA 10930Hinode XRT image21:30:32UT2006.12.12
Extrapolated field lines based on vector magnetogram observed byHinode SOT SP
2006.12.12 20:30-21:33UTFOV:295.20 x 162.30 arcsec
Compared with coronal image observed by XRT NOAA 10930Compared with coronal image observed by XRT NOAA 10930
Central domain of the extrapolated Central domain of the extrapolated fieldfield
NOAA 10930NOAA 10930
During the flare
Before the flare
ThanksThanks