1. RHESSI and the Solar Flare X-ray Spectrum Ken Phillips Presentation at Wroclaw Workshop “ X-ray spectroscopy and plasma diagnostics from the RESIK, RHESSI and SPIRIT Instruments “, December 6—8, 2005

2. Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI)

3. RHESSI Launch from Pegasus Launch of RHESSI: Feb. 5, 2002 Pegasus rocket carrying RHESSI NASA plane

4. RHESSI Spacecraft Concept SUN S/C Rotates

5. RHESSI’s Energy Range RHESSI’s Energy Range RHESSI observes soft and hard X-ray emission up to gamma-rays: 4 keV up to 17 MeV RHESSI observes soft and hard X-ray emission up to gamma-rays: 4 keV up to 17 MeV Conversion is Conversion is λ(Å) = 12.4 / E (keV) λ(Å) = 12.4 / E (keV)

6. RHESSI 10—25 keV images of near-limb flare RHESSI 10—25 keV images of near-limb flare LinHui Sui & Holman 2003 Spatial resolution in these images 7 arcsec (can be as good as 2 arcsec) Solar Limb

7. Holman et al. (2002) -- HXR and Gamma-ray images -- RHESSI, 2002 July 23 flare Gamma rays HXR emission SOHO/MDI magnetogram

8. TRACE and RHESSI Flare Images TRACE and RHESSI Flare Images

9. RHESSI as a Spectrometer: Spectral Resolution RHESSI as a Spectrometer: Spectral Resolution

10. . Spectral resolution best for RHESSI Detectors 3 and 4: 1 keV at ~ 7 keV Spectral resolution best for RHESSI Detectors 3 and 4: 1 keV at ~ 7 keV or ~0.25Å at 1.9Å. or ~0.25Å at 1.9Å. Spectral resolution “broad-band”, not like crystal spectrometer resolution. Spectral resolution “broad-band”, not like crystal spectrometer resolution. RHESSI sees Fe XXV lines and satellites as a single “bump” on continuum. RHESSI sees Fe XXV lines and satellites as a single “bump” on continuum. However, RHESSI does see the continuum (whereas crystal spectrometers usually affected by crystal fluorescence). However, RHESSI does see the continuum (whereas crystal spectrometers usually affected by crystal fluorescence).

11. RHESSI flare spectrum RHESSI flare spectrum

12. Flare X-ray Spectra Flare X-ray Spectra Electrons accelerated at reconnection site travel from loop top to chromosphere, producing X-ray emission with nonthermal spectrum (hv > 20 keV). Electrons accelerated at reconnection site travel from loop top to chromosphere, producing X-ray emission with nonthermal spectrum (hv > 20 keV). Material in previously empty loop filled with heated plasma (T~20MK) that produces a thermal spectrum (hv < 20 keV) consisting of lines and continuum. Material in previously empty loop filled with heated plasma (T~20MK) that produces a thermal spectrum (hv < 20 keV) consisting of lines and continuum.

13. Two Line features in RHESSI spectra 6.7 keV or “Fe line feature” –Fe XXV lines –Fe XVIII – Fe XXIV satellites –Fe XXVI lines at higher T (>80MK) –Seen with crystal spectrometers 8 keV or “Fe/Ni line feature” –More highly excited Fe XXV,Fe XXVI lines –Ni XXVII, Ni XXVIII lines & satellites –Never seen with crystal spectrometers

14. Fe and Fe/Ni line features: RHESSI observations So RHESSI the first instrument (apart from NEAR-PIN) to see the 8 keV feature By analyzing the 2 line features, one can diagnose the hottest part of the flare thermal plasma

15. Chianti Spectrum,T=20MK Fe XXV +satellites Ni XXVII + sats Ca XIX Fe XXV Fe edge Fe XXV Fe XXVI

16. Chianti spectra + spectra smoothed to RHESSI resolution Chianti spectra + spectra smoothed to RHESSI resolution

17. SMM/BCS Fe line flare spectra Fluorescence background

18. Synthetic (CHIANTI) spectra, solar plasma (8-33 MK) Synthetic (CHIANTI) spectra, solar plasma (8-33 MK) RHESSI (1 keV) resolution assumed Chianti: coronal abund. + Mazzotta et al. ion. eq.

19. Lines making up the `Fe-line’ (6.7 keV) feature Lines making up the `Fe-line’ (6.7 keV) feature

20. Lines making up the `Fe/Ni’ (8 keV) feature Lines making up the `Fe/Ni’ (8 keV) feature

21. Solar flare spectrum, NEAR- PIN and Yohkoh/BCS Solar flare spectrum, NEAR- PIN and Yohkoh/BCS NEAR-PIN: R. Starr Yohkoh: S, Ca, Fe channels NEAR-PIN BCS Fe line (6.7 keV) Fe/Ni line (8 keV) S XV Ca XIX

22. Element (e.g. Fe) Abundances With measurement of line and continuum flux, we can measure element abundances With measurement of line and continuum flux, we can measure element abundances Thus, with 6.7 keV (“Fe line”) feature, we can measure Fe/H. Thus, with 6.7 keV (“Fe line”) feature, we can measure Fe/H. Use equivalent width of line to do this. Use equivalent width of line to do this.

23. Emission Line Equivalent Width Definition Energy (keV)

24. Equivalent Width of the Fe line Based on Chianti v. 5.1, coronal abundances and Mazzotta et al. ion fractions (This plot is different from Phillips 2004)

25. RESIK in 3 rd order Attenuator states

27. Theoretical curve (Phillips 2004) based on coronal Fe abundance and Mazzotta et al. ion fractions

28. FeFeFeFe Theoretical curve

29. Equivalent Width Plots Equivalent Width Plots April 23, 2003 flare is `good’ example – plenty of not-so-good examples! April 23, 2003 flare is `good’ example – plenty of not-so-good examples! There are problems associated with high count rates in the A0 attenuator state and in the A3 attenuator state – these are not understood at present. There are problems associated with high count rates in the A0 attenuator state and in the A3 attenuator state – these are not understood at present. Cristina will show more examples…. Cristina will show more examples…. Tentative conclusion: flare Fe abundance ~ coronal Fe abundance (Feldman & Laming 2000) Tentative conclusion: flare Fe abundance ~ coronal Fe abundance (Feldman & Laming 2000)

30. Fe XXIV/Fe XXV Ion Fractions wrong? In CHIANTI analysis, we used Mazzotta et al. (1998) ion fractions – maybe slightly wrong? In CHIANTI analysis, we used Mazzotta et al. (1998) ion fractions – maybe slightly wrong? No measured rates for these ions, so everything relies on calculations No measured rates for these ions, so everything relies on calculations There are some ‘measured’ rates from SMM/BCS flare spectra: Fe XXIV satellites (j and q) / Fe XXV w line ratios (Antonucci et al.) There are some ‘measured’ rates from SMM/BCS flare spectra: Fe XXIV satellites (j and q) / Fe XXV w line ratios (Antonucci et al.)

31. RHESSI and CORONAS-F/RESIK Solar Flare Spectra Both RHESSI and RESIK spectrometers carefully calibrated – estimated uncertainties ~20% Both RHESSI and RESIK spectrometers carefully calibrated – estimated uncertainties ~20% Useful to compare spectra for same times in flares – agreement very good. Useful to compare spectra for same times in flares – agreement very good. RESIK 1 st -order spectra agree with the low-energy end of RHESSI spectra. RESIK 1 st -order spectra agree with the low-energy end of RHESSI spectra.

32. Plotting spectra from 7 RHESSI detectors + RESIK

33. Summary and Conclusions RHESSI a `broad-band’ spectrometer, sees both thermal and nonthermal spectra of solar flares (sp. res. 1 keV). RHESSI a `broad-band’ spectrometer, sees both thermal and nonthermal spectra of solar flares (sp. res. 1 keV). RHESSI sees two line features, at 6.7 keV (Fe) and 8 keV (Fe/Ni). RHESSI sees two line features, at 6.7 keV (Fe) and 8 keV (Fe/Ni). Line equivalent widths mostly indicate coronal abundance of Fe. Line equivalent widths mostly indicate coronal abundance of Fe. Possibly ionization fractions of Fe XXV need revision. Possibly ionization fractions of Fe XXV need revision.