Reconstruction of the EUV spectral irradiance Atomic data and model atmosphere structures Margit Haberreiter Veronique Delouille, Benjamin Mampeay, Micha Schoell, Rami Qahwaji, Ilaria Ermolli SOLID First Annual Meeting Margit Haberreiter Oct 14 – 18, 2013, Orléans

Reconstruction of EUV variations SOLID First Annual Meeting Margit Haberreiter Oct 14 – 18, 2013, Orléans i: concentric rings r i j: class (feature) I j :(r i,λ): Intensity for each feature and position on the solar disk

SOLID First Annual Meeting Margit Haberreiter Oct 14 – 18, 2013, Orléans I(λ,μ,φ,t) n level, n el,n ion,… (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 Haberreiter Oct 14 – 18, 2013, Orléans 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 Haberreiter Oct 14 – 18, 2013, Orléans

SolMod Contrast at EIT passbands SOLID First Annual Meeting Margit Haberreiter Oct 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 Haberreiter Oct 14 – 18, 2013, Orléans

Filling factors from SOHO/EIT SOLID First Annual Meeting Margit Haberreiter Oct 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 Haberreiter Oct 14 – 18, 2013, Orléans

SolMod Reconstruction versus SOHO/SEM SOLID First Annual Meeting Margit Haberreiter Oct 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 Haberreiter Oct 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 AD With AD

SOLID First Annual Meeting Margit Haberreiter Oct 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 Haberreiter Oct 14 – 18, 2013, Orléans Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A

SOLID First Annual Meeting Margit Haberreiter Oct 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 Haberreiter Oct 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 Haberreiter Oct 14 – 18, 2013, Orléans Two main points to be addressed: 1.Update of atomic data of already implemented spectral lines to Chianti 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 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 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 SOLID First Annual Meeting Margit Haberreiter Oct 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

Deliverables within first year of SOLID (1) NoTitleLead Benficiary MonthStatus D4.2Improved atmosphere structures for the synthesis of the EUV/UV spectrum PMOD/WR C 6 -> 12 ( ✔ ) Ly α In progress (He II) D4.3Improvement of the atomic data set employed in the spectral synthesis PMOD/WR C 12 (✔)(✔) D4.4Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images PMOD/WR C 12In progress D8.1Project WebpagePMOD/WR C 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 Haberreiter Oct 14 – 18, 2013, Orléans D4.2: 2. He continuum and He II 304 Å Haberreiter (2011), Solar Physics, 274, 473