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Studies on the 2002 July 23 Flare with RHESSI

Studies on the 2002 July 23 Flare with RHESSI. Ayumi ASAI Solar Seminar, 2003 June 2. RHESSI ( レッシ ) R euven R amaty H igh E nergy S olar S pectrospic I mager. Launched on 2002 Feburary 5 weight : 290kg length : 2.2m (solar panel : 5.7m) cost : ～ 70M$. RHESSI.

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Studies on the 2002 July 23 Flare with RHESSI

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  1. Studies on the 2002 July 23 Flare with RHESSI Ayumi ASAI Solar Seminar, 2003 June 2

  2. RHESSI (レッシ)Reuven Ramaty High Energy Solar Spectrospic Imager Launched on 2002 Feburary 5 weight : 290kg length : 2.2m (solar panel : 5.7m) cost : ～70M$

  3. RHESSI • energy range : 3 keV – 17 MeV • imaging maximum spatial resolution : beam size : 3.”3 FWHM • spectroscopy high spectral resolution : 1~10 keV

  4. 2002 July 23 Flare • 2002-July-23 00:15UT • GOES X4.8 • NOAA 0039 • (near south-east limb) GOES flux Ha image taken with Sartorius Telescope NoRH 17GHz NoRH 34GHz 00:00 01:00 02:00

  5. EUV(195Å)像 EUV (195Å) images obtained with TRACE East West

  6. The Determination and Use of Mean Electron Flux Spectra in Solar Flares J.C. Brown The Injected Power in Solar Flare Bremsstrahlung-Producing Electrons - Death to the 'Low Energy Cutoff A.G. Emslie RHESSI Imaging Spectroscopy of the Large Gamma-Ray Flare of July 23, 2002 A.G. Emslie H-alpha line polarization in the major flare of 2002 July 23 I. Observations and data analysis N. Firstova Why there was no Solar Energetic Particle Event Associated with the RHESSI Flare of 2002 July 23? N. Gopalswamy Electron Bremsstrahlung Hard X-ray Spectra, Electron Distributions and Energetics in the 2002 July 23 Solar Flare G.D. Holman First gamma-ray images of a solar flare G.J. Hurford Explanations for Deviations from Power-Law Behavior in the Hard X-ray Spectrum of the July 23, 2002 Solar Flare E.P. Kontar Hard X-ray sources and motions in the July 23, 2002 gamma-ray flareS. Krucker Bob Lin's opus Implications of RHESSI Neutron-Capture Line Measurements on the Photospheric 3He/H ratio and Particle Scattering in the Coronal Magnetic LoopR.J. Murphy Regularized Dynamic Electron Flux Spectra in the July 23, 2002 Solar FlareM. Piana High-resolution observation of the solar positron-electron annihilation lineG.H. Share Directionality of flare-associated alpha-particles at the Sun G.H. Share High-Resolution Spectroscopy of Gamma-Ray Lines from the X-Class Solar Flare of 23 July, 2002 D.M. Smith RHESSI observation of the 1809 keV line from Galactic 26Al D.M. Smith Radio and hard X-ray images of high-energy electrons in a compact X-class solar flareS.M. White Paper List 17 papers!

  7. The Determination and Use of Mean Electron Flux Spectra in Solar Flares J.C. Brown The Injected Power in Solar Flare Bremsstrahlung-Producing Electrons - Death to the 'Low Energy Cutoff A.G. Emslie RHESSI Imaging Spectroscopy of the Large Gamma-Ray Flare of July 23, 2002 A.G. Emslie H-alpha line polarization in the major flare of 2002 July 23 I. Observations and data analysis N. Firstova Why there was no Solar Energetic Particle Event Associated with the RHESSI Flare of 2002 July 23? N. Gopalswamy Electron Bremsstrahlung Hard X-ray Spectra, Electron Distributions and Energetics in the 2002 July 23 Solar Flare G.D. Holman First gamma-ray images of a solar flare G.J. Hurford Explanations for Deviations from Power-Law Behavior in the Hard X-ray Spectrum of the July 23, 2002 Solar Flare E.P. Kontar Hard X-ray sources and motions in the July 23, 2002 gamma-ray flareS. Krucker Bob Lin's opus Implications of RHESSI Neutron-Capture Line Measurements on the Photospheric 3He/H ratio and Particle Scattering in the Coronal Magnetic LoopR.J. Murphy Regularized Dynamic Electron Flux Spectra in the July 23, 2002 Solar FlareM. Piana High-resolution observation of the solar positron-electron annihilation lineG.H. Share Directionality of flare-associated alpha-particles at the Sun G.H. Share High-Resolution Spectroscopy of Gamma-Ray Lines from the X-Class Solar Flare of 23 July, 2002 D.M. Smith RHESSI observation of the 1809 keV line from Galactic 26Al D.M. Smith Radio and hard X-ray images of high-energy electrons in a compact X-class solar flareS.M. White Paper List

  8. Imaging Krucker et al. (2003) ApJL • 4 HXR sources • 3 footpoint sources (> 30keV) • 1 coronal sources (<30 keV) • comparison between their positions with those of EUV(TRACE)/Ha sources • footpoint sources  flare ribbons • coronal sources  above post-flare loops

  9. HXR Sources

  10. Evolution of HXR Sources f3 f1 velocity count

  11. Radio Sources White et al. (2003) ApJ • Radio data : Nobeyama NoRH

  12. 12-20keV TRACE • 17 GHz sources are co-spatial with coronal HXR sources 17GHz 12-20keV 100-150keV

  13. g-Ray Imaging Hurford et al. (2003) ApJ • This flare is the first, and the only one so far, g-ray line event • direct indication of the spatial properties of accelerated ions near the sun • 2.223 MeV line … • narrow deuterium line (neutron capture) • dense plasma (chromosphere) • red-shifted  precipitation

  14. g-Ray Lines • ion acceleration • collisions with the solar atmosphere excited nuclei emit prompt nuclear de-excitation lines • secondary process neutron capture line (2.223 MeV) positron-annihilation line (511 keV)

  15. Imaging of g-Ray Source sun

  16. No Brightening in Ha 1s circle error : 6”

  17. Discussions • 2.2 MeV source was found to be displaced from the main bright point there are significant differences in location and/or morphology between the electron- and ion-associated sources • ion- and electron-light curves are similar to each other common acceleration process

  18. Spectroscopy Holman et al. (2003) ApJ • integrated photon flux spectra :10-300 keV • fitting isothermal + double power low (nonthermal) • electron flux distribution thin-target / thick-target • energy content

  19. Fitting 100keV 10keV

  20. Evolution of T / EM temperature GOES emission measure

  21. Thick-Target electron indices

  22. Energetics GOES RHESSI nonthermal

  23. Discussions • fitting of nonthermal electron : • double poewr law distribution with low energy cut-off : 20-40 keV • minimum total energy deposited by nonthermal electrons : 2.6×1031 erg comparable to thermal energy input require imaging spectroscopy

  24. Imagin Spectroscopy Emslie et al. (2003) ApJ • Evolution of spectra at 4 HXR sources • Temperature, Emission measure M N C S

  25. fitting C : thermal N, S, M : nonthermal

  26. T coronal source (C) • temperature K • EM J • softer spectral index than footpoint sources (N,S,M) EM

  27. Summary • Flare studies with RHESSI • Imaging, Spectroscopy … • other big flares … ? • 2003 Mar 17/18 • 2003 May 27/28/29 • 18th paper on July 23, 2002 flare (by Asai et al.) ?

  28. Double Power Low indices single power law break energy

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