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EUV Spectral Synthesis and Reconstruction
Margit Haberreiter, PMOD/WRC, Davos, Switzerland
Cis Verbeeck, Veronique Delouille, Rami Qahwaji, Ilaria Ermolli
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Deliverables of PMOD
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Involvement of PMOD in WP8
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I(λ,μ,φ,t)
nlevel, nel,nion,…
(x,y,z,t)
I(λ,μ,φ,t)
Iterative
process
EUV reconstruction - Semi-empirical modeling
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Solar Modeling (SolMod)
• Multi level atoms– 373 ions, from H to Ni with ioncharge 25– ~14’000 atomic levels– ~170’000 spectral lines – Statistical equation is solved to get the level populations
• Chromosphere and transition region – for ioncharge 2: – full NLTE (Fontenla et al., 2006; 2007; 2009)
– plus optically thin transition region lines– Spherical symmetry
• Corona– ioncharge >2 – optically thin, i.e. collisions and spontaneous emission– Line of sight integration accounts for opacity– Spherical symmetry
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1D Atmosphere StructuresPhotosphere and Chromosphere
0.1 1 10 100 1 103
1 104
1 105
4000
6000
8000
B 1001D 1002F 1003H 1004P 1005
B 1001D 1002F 1003H 1004P 1005
Pressure (dyn cm^-2)
Tem
pera
ture
(K
)
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1D Atmosphere Structures - Corona
5 104 1 10
5 1.5 105 2 10
5
1 106
2 106
3 106
SRPM - Quiet Sun ISRPM - Quiet Sun IISRPM - Quiet Sun IIISRPM - Network RegionSRPM - Active RegionCranmer - Equatorial HoleCranmer - Active RetionCranmer - Polar Region
Height (km)
Tem
pera
ture
(K
)
• SRPM Models are based on Doschek (1997), ApJ, 476, 903, Singh et al., 1982, J. Astrophys. 3, 249• Cranmer et al, 2007, ApJS 171, 520
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Spherical Symmetry
Allows the calculation
of intensities at and beyond the limb
Up to a factor of 2!
Account for corona over
Up to 1.4 Solar Radii
(e.g. Haberreiter et al. 2008)
Adopted from Mihalas, 1978
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SWAP integrated intensities
SWAP data courtesy Anik de Groof
Mean of off-limb contribution: 35%
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1. Photosphere/ChromosphereSegmentations Masks from PSPT
Disk mask on 2005/9/12 obtained from PSPT data, Mauna Loa, Hawaiihttp://lasp.colorado.edu/pspt_access/
(R) Sunspot Penumbra(S) Sunspot Umbra(P) Faculae(H) Plage(F) Active network(D) Quiet network (white)
(B) Intergranular Cells
Determined by the contrast as a function of the position on the disk- Only possible with respect to a - normalized quiet Sun intensity
Continuum, 607 nm
Ca II 393.4, FWHM=0.27nm
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June 1, 2003
Coronal Hole Mask Active Region Mask
SPoCA Image Decomposition: Cis Verbeeck, ROB
2. Corona - Segmentation of EIT images
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Calculation versus observed EVE spectrum
Fontenla et. al. 2009, ApJ
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Comparison to SDO/EVE observations
Haberreiter, 2011, Solar Physics, 274, 473
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Comparison to EVE observations II
ROB Seminar, Sept 26, 2011 Margit Haberreiter
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Comparison to EVE observations III
ROB Seminar, Sept 26, 2011 Margit Haberreiter
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Synthetic EUV Spectra
50 1001 10
7
1 106
1 105
1 104
1 103
0.01
0.1
1
SPRM 1SPRM 2SPRM 3SPRM 4SPRM 5
Wavelength (nm)
Irra
dian
ce (
erg
cm-2
s-1
nm
-1)
Quiet CoronaQuiet Coronal NetworkActive Coronal NetworkHot loops Super hot loops
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17/30
Scheme for Spectral Irradiance Reconstruction
1. Intensity spectra are calculated for different positions on the solar disk
2. Spectra are weighted based on the relative area coverage of different solar features for different posititions on the solar disk
3. Result: Spectral variability for various time-scales over a broad wavelength range
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EIT analysis 1997 - 2011
Data from Barra et al, 20d t9 Verbeeck et al, 2013, submitted to A&A
Based on EIT 171 and 195 A imagesBoth data sets for disk center
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Reconstruction of the EUV for solar cycle 23
Haberreiter, 2012, IAU Symposium 286
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Reconstruction of the EUV for solar cycle 23
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EUV Reconstruction vs SEM Data
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TIMED/SEE vs SOHO/SEM Data
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Test case for EUV reconstruction
SOLID Kick-off Meeting Margit Haberreiter
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EUV reconstruction for test period
SOLID Kick-off Meeting Margit Haberreiter
*1.2
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LYRA passbands
LYRA CH 3: 17-80 nmLYRA CH 4: 6-20 nm
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Deliverables of PMOD
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Involvement of PMOD in WP8
Which of the existing reconstructions will be included in the final SSI time series