EUV Spectral Synthesis and Reconstruction Margit Haberreiter, PMOD/WRC, Davos, Switzerland Cis Verbeeck, Veronique Delouille, Rami Qahwaji, Ilaria Ermolli

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<p>Phnomene der Sonne</p> <p>EUV Spectral Synthesis and Reconstruction Margit Haberreiter, PMOD/WRC, Davos, SwitzerlandCis Verbeeck, Veronique Delouille, Rami Qahwaji, Ilaria Ermolli 1TO do:</p> <p>Deliverables of PMOD</p> <p>Involvement of PMOD in WP8I(,,,t)nlevel, nel,nion,(x,y,z,t)I(,,,t)</p> <p>Iterative process</p> <p>EUV reconstruction - Semi-empirical modeling</p> <p>4Solar Modeling (SolMod)Multi level atoms373 ions, from H to Ni with ioncharge 25~14000 atomic levels~170000 spectral lines Statistical equation is solved to get the level populationsChromosphere and transition region for ioncharge 2: full NLTE (Fontenla et al., 2006; 2007; 2009)plus optically thin transition region linesSpherical symmetryCoronaioncharge &gt;2 optically thin, i.e. collisions and spontaneous emissionLine of sight integration accounts for opacitySpherical symmetry551D Atmosphere StructuresPhotosphere and Chromosphere</p> <p>61D Atmosphere Structures - Corona</p> <p>SRPM Models are based on Doschek (1997), ApJ, 476, 903, Singh et al., 1982, J. Astrophys. 3, 249Cranmer et al, 2007, ApJS 171, 5207Spherical SymmetryAllows the calculation of intensities at and beyond the limb</p> <p>Up to a factor of 2!</p> <p>Account for corona over Up to 1.4 Solar Radii</p> <p>(e.g. Haberreiter et al. 2008)Adopted from Mihalas, 1978</p> <p>8</p> <p>SWAP integrated intensitiesSWAP data courtesy Anik de GroofMean of off-limb contribution: 35%1. Photosphere/ChromosphereSegmentations Masks from PSPTDisk 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 CellsDetermined by the contrast as a function of the position on the diskOnly possible with respect to a normalized quiet Sun intensity</p> <p>Continuum, 607 nmCa II 393.4, FWHM=0.27nm10</p> <p>June 1, 2003Coronal Hole MaskActive Region MaskSPoCA Image Decomposition: Cis Verbeeck, ROB2. Corona - Segmentation of EIT imagesCalculation versus observed EVE spectrum</p> <p>Fontenla et. al. 2009, ApJComparison to SDO/EVE observations</p> <p>Haberreiter, 2011, Solar Physics, 274, 473Comparison to EVE observations IIROB Seminar, Sept 26, 2011 Margit Haberreiter</p> <p>Comparison to EVE observations IIIROB Seminar, Sept 26, 2011 Margit Haberreiter</p> <p>Synthetic EUV Spectra</p> <p>Quiet CoronaQuiet Coronal NetworkActive Coronal NetworkHot loops Super hot loops 1617/30Scheme for Spectral Irradiance ReconstructionIntensity spectra are calculated for different positions on the solar disk</p> <p>Spectra are weighted based on the relative area coverage of different solar features for different posititions on the solar disk </p> <p>3. Result: Spectral variability for various time-scales over a broad wavelength range</p> <p>EIT analysis 1997 - 2011Data from Barra et al, 20d t9 Verbeeck et al, 2013, submitted to A&amp;ABased on EIT 171 and 195 A imagesBoth data sets for disk centerReconstruction of the EUV for solar cycle 23Haberreiter, 2012, IAU Symposium 286</p> <p>Assumptions:</p> <p>Coronal 19</p> <p>Reconstruction of the EUV for solar cycle 23EUV Reconstruction vs SEM Data</p> <p>TIMED/SEE vs SOHO/SEM Data</p> <p>Test case for EUV reconstructionSOLID Kick-off Meeting Margit Haberreiter</p> <p>EUV reconstruction for test periodSOLID Kick-off Meeting Margit Haberreiter</p> <p>*1.2LYRA passbands</p> <p>LYRA CH 3: 17-80 nmLYRA CH 4: 6-20 nm</p> <p>Deliverables of PMOD</p> <p>Involvement of PMOD in WP8Which of the existing reconstructions will be included in the final SSI time series </p>