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EUV Spectral Synthesis and Reconstruction

Margit Haberreiter, PMOD/WRC, Davos, Switzerland Cis Verbeeck, Veronique Delouille, Rami Qahwaji , Ilaria Ermolli. EUV Spectral Synthesis and Reconstruction . Deliverables of PMOD. Involvement of PMOD in WP8. EUV reconstruction - Semi-empirical modeling. Iterative process.

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EUV Spectral Synthesis and Reconstruction

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  1. Margit Haberreiter, PMOD/WRC, Davos, Switzerland Cis Verbeeck, Veronique Delouille, RamiQahwaji, IlariaErmolli EUV Spectral Synthesis and Reconstruction

  2. Deliverables of PMOD

  3. Involvement of PMOD in WP8

  4. EUV reconstruction - Semi-empirical modeling Iterative process nlevel, nel,nion,… (x,y,z,t) I(λ,μ,φ,t) I(λ,μ,φ,t)

  5. SolarModeling (SolMod) 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 for ioncharge  2: full NLTE (Fontenla et al., 2006; 2007; 2009) plus optically thin transition region lines Spherical symmetry Corona ioncharge >2 optically thin, i.e. collisions and spontaneous emission Line of sight integration accounts for opacity Spherical symmetry

  6. 1D Atmosphere StructuresPhotosphere and Chromosphere

  7. 1D Atmosphere Structures - Corona • SRPM Models are based on Doschek (1997), ApJ, 476, 903, Singh et al., 1982, J. Astrophys. 3, 249 • Cranmer et al, 2007, ApJS 171, 520

  8. Spherical Symmetry Allowsthecalculation of intensities at and beyondthelimb Up to a factor of 2! Accountforcoronaover Up to 1.4 Solar Radii (e.g. Haberreiter et al. 2008) Adopted from Mihalas, 1978

  9. SWAP data courtesy Anik de Groof SWAP integrated intensities • Mean of off-limb contribution:  35%

  10. 1. Photosphere/ChromosphereSegmentationsMasks from PSPT Continuum, 607 nm Disk mask on 2005/9/12 obtained from PSPT data, Mauna Loa, Hawaii http://lasp.colorado.edu/pspt_access/ (R) Sunspot Penumbra (S) Sunspot Umbra (P) Faculae (H) Plage (F) Activenetwork (D) Quietnetwork (white) (B) IntergranularCells • Determinedbythecontrast as a • function of theposition on the disk • Onlypossiblewithrespect to a • normalizedquiet Sun intensity Ca II 393.4, FWHM=0.27nm

  11. 2. Corona -Segmentationof EIT images June 1, 2003 Coronal Hole Mask Active Region Mask SPoCA Image Decomposition: Cis Verbeeck, ROB

  12. Calculationversusobserved EVE spectrum Fontenla et. al. 2009, ApJ

  13. Comparison to SDO/EVE observations Haberreiter, 2011, Solar Physics, 274, 473

  14. ROB Seminar, Sept 26, 2011 Margit Haberreiter Comparison to EVE observations II

  15. ROB Seminar, Sept 26, 2011 Margit Haberreiter Comparison to EVE observations III

  16. Synthetic EUV Spectra Quiet Corona Quiet Coronal Network Active Coronal Network Hot loops Super hot loops

  17. Scheme for Spectral Irradiance Reconstruction • Intensity spectra are calculated for different positions on the solar disk • Spectra are weighted based on the relative area coverage of different solar features for different posititions on the solar disk 3. Result: Spectral variability for various time-scales over a broad wavelength range

  18. EIT analysis 1997 - 2011 Based on EIT 171 and 195 A images Both data sets for disk center Data from Barra et al, 20d t9 Verbeeck et al, 2013, submitted to A&A

  19. Reconstruction of the EUV for solar cycle 23 Haberreiter, 2012, IAU Symposium 286

  20. Reconstruction of the EUV for solar cycle 23

  21. EUV Reconstruction vs SEM Data

  22. TIMED/SEE vs SOHO/SEM Data

  23. SOLID Kick-off Meeting Margit Haberreiter Test case for EUV reconstruction

  24. SOLID Kick-off Meeting Margit Haberreiter EUV reconstruction for test period *1.2

  25. LYRA passbands LYRA CH 3: 17-80 nm LYRA CH 4: 6-20 nm

  26. Deliverables of PMOD

  27. Involvement of PMOD in WP8 • Whichof theexistingreconstructions will beincludedin thefinal SSI time series

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