Reconstruction of the EUV spectral irradiance Atomic data

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 Oct 14 – 18, 2013, Orléans Margit Haberreiter

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

EUV reconstruction - Semi-empirical modeling nlevel, nion, … Population numbers, Radiation field (x, y, z, t) Atomic physics, collisional and radiative rates, abundances SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Synthetic Spectrum I(λ, μ, φ, t) Iterative process Observed Spectrum Update of Physical Models T(z), ne(z), nh(z) Margit Haberreiter I(λ, μ, φ, t)

Solar Modeling (Sol. Mod) 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, So. Ph) – ioncharge >2 – optically thin, i. e. collisions and spontaneous emission (updated to latest Chianti v 7. 1. 9) – Line of sight integration accounts for opacity – Spherical symmetry

Model Atmospheres of Chromosphere and Transition region

Synthetic EUV Spectra Quiet Corona (QS 1) Quiet Coronal Network (QS 2) Active Coronal Network (AR 1) Hot loops (AR 2) Super hot loops (AR 3) SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Contribution of chromosphere, transition region and corona SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Sol. Mod Contrast at EIT passbands Contrast of SOLMOD spectra for the EIT 171 and 195 passbands SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Determination of the intensity centers for each class SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Filling factors from SOHO/EIT Image segmentation of SOHO/ EIT images carried out by ROB (D 3. 2) SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Sol. Mod Reconstruction versus SOHO/SEM SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Sol. Mod Reconstruction versus SOHO/SEM Missing some variability AR 2 and AR 3 are represented by the brightest model (AR 3) Reasons: Background radiation from chromosphere and transition region needs to be added In process for D 4. 4: using the PSPT filling factors Also analysis from Rami using the MDI analysis SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Pre-study: Determine the center intensity of each class Missing some variability: Some inter-class variation might be missing -> inherent to the approach SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Status of Deliverables under PMOD/WRCs’s responsibility • D 4. 2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum • D 4. 3 Improvement of the atomic data set employed in the spectral synthesis • D 4. 4 Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images • D 8. 2: Database to disseminate the irradiance time series and segmentation maps

D 4. 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)

D 4. 2: 1. Lyman-α line formation Without AD With AD Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A AD: Ambipolar Diffussion

D 4. 2: 1. Lyman-α line formation Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

D 4. 2: 1. Lyman-α line formation Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

D 4. 2: 2. He continuum and He II 304 Å Haberreiter, 2011, Solar Physics SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

D 4. 2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum • 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 SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

D 4. 3 Improvement of the atomic data set employed in the spectral synthesis • 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 SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

D 4. 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

D 4. 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

D 4. 3: 1. Update of atomic data of implemented spectral lines to Chianti 7. 1. 9 • For D 4. 3: • Compare the calculation of the additional optically thin lines carried out with SOLMOD versus CHIANTI SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter

Status Update WP 8 / SOLID Database http: //projects. pmodwrc. ch/solid-visualization/makeover/

Deliverables within first year of SOLID (1) No Title Lead Benficiary Month D 4. 2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum PMOD/WR 6 -> 12 C D 4. 3 Improvement of the atomic data set employed in the spectral synthesis PMOD/WR 12 C D 4. 4 Reconstruction and validation of PMOD/WR 12 EUV/UV Spectral irradiance based C on SOHO/EIT, PSPT/Ca II images D 8. 1 Project Webpage PMOD/WR 12 C Status (✔ ) Ly α In progress (He II) (✔ ) In progress ✔

Future Steps • Use PROBA 2/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

D 4. 2: 2. He continuum and He II 304 Å Haberreiter (2011), Solar Physics, 274, 473 SOLID First Annual Meeting Oct 14 – 18, 2013, Orléans Margit Haberreiter