Reconstruction of the EUV spectral irradiance Atomic data and model atmosphere structures Margit Haberreiter Veronique Delouille, Benjamin Mampeay, Micha.

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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, Orlans Slide 2 Reconstruction of EUV variations SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans i: concentric rings r i j: class (feature) I j :(r i,): Intensity for each feature and position on the solar disk Slide 3 SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans I(,,,t) n level, n el,n ion, (x,y,z,t) I(,,,t) Iterative process EUV reconstruction - Semi-empirical modeling Slide 4 Solar Modeling (SolMod) code Multi level atoms 373 ions, from H to Ni with ioncharge 25 ~14000+ atomic levels ~170000+ 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 Slide 5 Model Atmospheres of Chromosphere and Transition region Slide 6 Synthetic EUV Spectra SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Quiet Corona (QS1) Quiet Coronal Network (QS2) Active Coronal Network (AR1) Hot loops (AR2) Super hot loops (AR3) Slide 7 Contribution of chromosphere, transition region and corona SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Slide 8 SolMod Contrast at EIT passbands SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Contrast of SOLMOD spectra for the EIT 171 and 195 passbands Slide 9 Determination of the intensity centers for each class SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Slide 10 Filling factors from SOHO/EIT SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Image segmentation of SOHO/ EIT images carried out by ROB (D3.2) Slide 11 SolMod Reconstruction versus SOHO/SEM SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Slide 12 SolMod Reconstruction versus SOHO/SEM SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans 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 Slide 13 Pre-study: Determine the center intensity of each class SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Missing some variability: Some inter-class variation might be missing -> inherent to the approach Slide 14 Status of Deliverables under PMOD/WRCss 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 Slide 15 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- He II 304 nm in progress He II continuum (improvement not explicitly specified in the proposal) Slide 16 D4.2: 1. Lyman- line formation Schll, Haberreiter, Schmutz, Shapiro, submitted to A&A AD: Ambipolar Diffussion Without AD With AD Slide 17 SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans D4.2: 1. Lyman- line formation Schll, Haberreiter, Schmutz, Shapiro, submitted to A&A Slide 18 D4.2: 1. Lyman- line formation SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Schll, Haberreiter, Schmutz, Shapiro, submitted to A&A Slide 19 SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans D4.2: 2. He continuum and He II 304 Haberreiter, 2011, Solar Physics Slide 20 D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans Improvement atmosphere structure for modeling the Lyman 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 Slide 21 D4.3 Improvement of the atomic data set employed in the spectral synthesis SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans 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 Slide 22 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 Slide 23 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 Slide 24 D4.3: 1. Update of atomic data of implemented spectral lines to Chianti 7.1.9 SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans For D4.3: Compare the calculation of the additional optically thin lines carried out with SOLMOD versus CHIANTI Slide 25 Status Update WP8 / SOLID Database http://projects.pmodwrc.ch/solid-visualization/makeover/ Slide 26 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 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 Slide 27 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 Slide 28 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 Slide 29 SOLID First Annual Meeting Margit Haberreiter Oct 14 18, 2013, Orlans D4.2: 2. He continuum and He II 304 Haberreiter (2011), Solar Physics, 274, 473

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