reconstruction of the euv spectral irradiance atomic data and model atmosphere structures margit...
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Reconstruction of the EUV spectral irradiance
Atomic data and model atmosphere
structures
Margit HaberreiterVeronique Delouille, Benjamin Mampeay, Micha Schoell, Rami Qahwaji, Ilaria Ermolli
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Reconstruction of EUV variations
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
i: concentric rings rij: class (feature)
Ij:(ri,λ): Intensity for each feature and position on the solar disk
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)
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
I(λ,μ,φ,t)
nlevel, nel,nion,…
(x,y,z,t)
I(λ,μ,φ,t)
Iterative
process
EUV reconstruction - Semi-empirical modeling
Solar Modeling (SolMod) code• 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 – Fontenla et al. ,2009 atmosphere structures -> to be
updated– for ioncharge 2: – full NLTE (Fontenla et al., 2009)
• Corona– Coronal structures (Haberreiter, 2011, SoPh)– ioncharge >2 – optically thin, i.e. collisions and spontaneous emission
(updated to latest Chianti v7.1.9)– Line of sight integration accounts for opacity– Spherical symmetry
Model Atmospheres of Chromosphere and Transition region
Synthetic EUV Spectra
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
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 Corona (QS1)Quiet Coronal Network (QS2)Active Coronal Network (AR1)Hot loops (AR2)Super hot loops (AR3)
Contribution of chromosphere, transition region and corona
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
SolMod Contrast at EIT passbands
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Contrast of SOLMOD spectra for the EIT 171 and 195 passbands
Determination of the intensity centers for each class
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Filling factors from SOHO/EIT
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Image segmentation of SOHO/ EIT images carried out by ROB(D3.2)
SolMod Reconstruction versus SOHO/SEM
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
SolMod Reconstruction versus SOHO/SEM
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Missing some variability
AR2 and AR3 are represented by the brightest model (AR3)
Reasons: Background radiation from chromosphere and transition region needs to be added
In process for D4.4: using the PSPT filling factors
Also analysis from Rami using the MDI analysis
Pre-study: Determine the center intensity of each class
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Missing some variability:
Some inter-class variation might be missing
-> inherent to the approach
Status of Deliverables under PMOD/WRCs’s responsibility
• D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum
• D4.3 Improvement of the atomic data set employed in the spectral synthesis
• D4.4 Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images
• D8.2: Database to disseminate the irradiance time series and segmentation maps
D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum
• Main problems indicated with the line formation of EUV/UV spectral lines
• Lyman-α ✔
• He II 304 nm in progress
• He II continuum
(“improvement” not explicitly specified in the proposal)
D4.2: 1. Lyman-α line formation
Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A
AD: Ambipolar Diffussion
Without ADWith AD
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
D4.2: 1. Lyman-α line formation
Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A
D4.2: 1. Lyman-α line formation
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
D4.2: 2. He continuum and He II 304 Å
Haberreiter, 2011, Solar Physics
D4.2 Improved atmosphere structures for the
synthesis of the EUV/UV spectrum
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
• Improvement atmosphere structure for modeling the Lyman α line
• Decreased temperature in the chromosphere will lead to a decrease in the He II 304 spectral line
• He II 30.4 nm calculations are on their way for end of November
D4.3 Improvement of the atomic data set employed in the spectral synthesis
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
• Two main points to be addressed:
1. Update of atomic data of already implemented spectral lines to Chianti 7.1.9
2. Implementation of highly ionized ions
3. Update from Giulio on important lines for the (optically think UV that were not yet implemented in Chianti 7.1.9
D4.3: 1. Update of atomic data of implemented spectral lines to Chianti
7.1.9
• Update of the atomic data set from Chianti 5.2 to Chianti 7.1.9
D4.3: 1. Update of atomic data of implemented spectral lines to Chianti 7.1.9
• Update of the atomic data set from Chianti 5.2 to Chianti 7.1.9
D4.3: 1. Update of atomic data of implemented spectral lines to
Chianti 7.1.9
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
• For D4.3:
• Compare the calculation of the additional optically thin lines carried out with SOLMOD versus CHIANTI
Status Update WP8 / SOLID Database
http://projects.pmodwrc.ch/solid-visualization/makeover/
Deliverables within first year of SOLID (1)
No Title Lead Benficiary
Month Status
D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum
PMOD/WRC
6 -> 12 (✔) Ly αIn
progress (He II)
D4.3 Improvement of the atomic data set employed in the spectral synthesis
PMOD/WRC
12 (✔)
D4.4 Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images
PMOD/WRC
12 In progress
D8.1 Project Webpage PMOD/WRC
12 ✔
Future Steps
• Use PROBA2/SWAP and PSPT filling factors for reconstruction of the EUV/UV and visible
• Use the MDI analysis by Rami for the reconstruction of the UV and visible
• Use Picard/SODISM data for reconstruction of the UV and visible
Towards the Recommended SSI time series
• SSI from semi-empirical modeling
• We need to discuss an approach how to determine the error propagation:
• the contrast of activity features
• filling factor
SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans
D4.2: 2. He continuum and He II 304 Å
Haberreiter (2011), Solar Physics, 274, 473