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Modelling the Solar UV variability

Modelling the Solar UV variability. M. Haberreiter ISSI Study Team on Solar Magnetism and Irradiance 11.-15.October 2004. Overview. Motivation Modeling the UV variability Non-LTE code COSI Limb calculation Reconstruction LYRA instrument Summary. S pectral ir radiance λ = 121.6 nm.

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Modelling the Solar UV variability

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  1. Modelling the Solar UV variability M. Haberreiter ISSI Study Team on Solar Magnetism and Irradiance 11.-15.October 2004 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  2. Overview • Motivation • Modeling the UV variability • Non-LTE code COSI • Limb calculation • Reconstruction • LYRA instrument • Summary Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  3. Spectral irradiance λ=121.6 nm SUSIM/UARS Data: Linton Floyd Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  4. Temperature and ozone sensitivity dT (mK/nm) dO3 (‰/nm) Rozanov et al. 2002, Proc. SOHO 11 Symp., 181 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  5. Irradiance variations Haberreiter et al. 2002, Proc. SOHO 11 Symp., 209 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  6. Identification of active regions 1. Magnetic flux  filling factor  2. Intensity contrast < 1 sunspot else  faculae th: threshold magnetic flux 3: magnetic fluxsaturation Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  7. Modeling spectral variability Intensity spectra calculated with COSI: • quiet sun • faculae • sunspots Magnetogram analysis: • time-dependent filling factorsfor faculae (+network) ,sunspots Variation of solar activity: Krivova & Solanki (2003) Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  8. facular and sunspot effective areas MDI magnetogramm continuum intensity image August 30, 1996 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  9. facular and sunspot effective areas maps for faculae for sunspots August 30, 1996: active region dominated by faculae Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  10. facular and sunspot effective areas (2) MDI magnetogramm continuum intensity image November 25, 1996 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  11. facular and sunspot effective areas (2) maps for faculae for sunspots November 25, 1996: faculae and sunspot extracted Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  12. Comparison with observations 1a 1b Fligge, Solanki Unruh 2000, A&A 353, 380 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  13. COSI - COde for Solar Irradiance • Updated version of the spherical radiative transfer code based on Schmutz W., 1997, A&A, 321,268 • Spectrum synthesis program SYNSPEC, based on Hubeny 1988, Hubeny & Lanz 2000 • atmosphere structure (p, T) by Fontenla et al. (1999) for quiet Sun, sunspots, faculae • spherical geometry Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  14. COSI – COde for Solar Irradiance • non-local thermodynamic equilibrium (non-LTE), important below 200 nm • non-LTE line blanketing with opacity distribution functions • Latest photoionization cross sections • C I, Mg I, Al I, Si I, Fe I (Haberreiter et al. 2002) • Opacity project (Seaton et al. 1994) • IRON project (Bautista & Pradhan 1997) Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  15. Temperature profiles Fontenla et al. 1999 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  16. Emission due to LTE and rising temperature H I  4863 - LTE Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  17. H I  4863 - NLTE Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  18. Hydrogen lines Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  19. Spherical symmetry plane-parallel spherical Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  20. Model P - plage Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  21. Model C – quiet Sun Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  22. Limb variation Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  23. Magnetogram Data Begin End • NSO/Kitt Peak Vacuum Telescope, Tucson • NSO/KP, 512nm 08 / 24 / 1974 04 / 07 / 1992 • NASA/NSO, 868nm 11 / 21 / 1992 12 / 22 / 2001 (05 / 18 / 1996) • MDI/SOHO 05 / 19 / 1996 04 / 17 / 2002 MDI: Michelson Doppler Imager Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  24. Daily Variability of Lyman  Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  25. Lyman  Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  26. Lyman  Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  27. LYRA 2005-2006 Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  28. LYRA 2005-2006 Optical Characteristics • 3 Detector-Head with 4 Channels Channel 1: 121.6 nm (Ly) Channel 2: 210-220 nm (Hertzberg continuum) Channel 3: 17-70 nm (He II) Channel 4: 1-20 nm Margit Haberreiter, PMOD/WRC, Davos, Switzerland

  29. PROBA2/LYRA spectral coverage Margit Haberreiter, PMOD/WRC, Davos, Switzerland

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