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Using Gamma Rays to Measure Accelerated Ions and Electrons and Ambient Composition

Using Gamma Rays to Measure Accelerated Ions and Electrons and Ambient Composition. Gerald Share 1,2 , Ronald Murphy 2 , Benz Kozlovky 3 , and Juergen Kiener 4. 1 UMD, 2 NRL, 3 Tel Aviv Univ, 4 Univ. Paris Sud. Supported under NASA Grants NNX07AH81G, NNX07AO74G, and NNG06GG14G.

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Using Gamma Rays to Measure Accelerated Ions and Electrons and Ambient Composition

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  1. Using Gamma Rays to Measure Accelerated Ions and Electrons and Ambient Composition Gerald Share1,2, Ronald Murphy2, Benz Kozlovky3, and Juergen Kiener4 1 UMD, 2NRL, 3Tel Aviv Univ, 4Univ. Paris Sud Supported under NASA Grants NNX07AH81G, NNX07AO74G, and NNG06GG14G.

  2. We have re-evaluated the SMM instrument response using a Monte Carlo calculation in lieu of the original quasi-empirical response. Two fits to the 1981 April 27 spectrum are shown below; both are acceptable but the fit with PL*Exp is favored. The latter compensates for the unresolved nuclear continuum that extends above 10 MeV Fit with PL + PL x exp: chi2/dof 1.008 (50% probability) Fit with PL + PL chi2/dof 1.053 (20% probability)

  3. We fit the flare spectra with the pl + plexp, 0.5, 2.2 MeV, a – 4He lines, a solar Compton-scattered 2.2 MeV continuum, individual line templates for p, a interactions on C, N, O, Ne, Mg, Si, and Fe, individual line templates for accelerated C, N, O, 3He, and a combined template (coronal composition normalized to Fe) for Ne, Mg, Si, and Fe on H and He. We have included a 5% systematic in the data >1 MeV and a 15% systematic between 1.9 and 2.4 MeV to account for the strong 2.2 MeV line and its back scatter peak that are not adequately represented by the detector response function. These nuclear line templates were calculated for heliocentric angle of the flare and for various values of a/p and spectral index (assuming the same index for all accelerated particles; no significant difference found when allowing the alphas and protons to have different indices.)

  4. Fits to the 1989 October 19 flare showing the total fit, bremsstrahlung, direct interaction (i.e. accelerated p and a on ambient elements), inverse interaction (i.e. heavy ions on ambient elements), a-4He, and 0.511/2.223 MeV line components and Compton-scattered 2.2 MeV line.

  5. 1981 April 27 chi2 contour plots for spectral index and /p ratio. From Monte Carlo studies a Dc2 = 3.5 has a 68% probability. Curve marked 186 shows the indices and /p ratios consistent with photospheric He/O (Asplund abundances) for the flux measured in the -4He fusion lines (the other dotted curves show the 1 sigma statistical uncertainty in the line measurement).

  6. Anders and Grevesse abundances requires a significantly higher accelerated alpha/proton ratio. The accelerated particles appear to have a power law index between ~3 and 4.

  7. In order to estimate the ambient abundances (normalized to O) for the flare we use the parameters for the best fitting /p ratio and spectral index consistent with the Asplund photospheric He/O. C/O ratio consistent with Anders & Grevese photospheric and coronal values; Ne/O is ~12% (note this is lower the value adopted by Ramaty et al.,) the low FIP elements do not appear to be significantly enhanced over photospheric values.

  8. The ambient C abundance relative to O for twelve SMM flares (errors include +- 1 sigma range in Asplund He/O. The average ratio appears to be consistent with both coronal and Anders and Grevesse photopheric abundances. It is significantly lower than the Asplund et al. photospheric abundance. No evidence for variability

  9. The ambient Ne abundance relative to O for twelve SMM flares. The average ratio appears to be consistent with a value between 15 and 20%, consistent with adopted photospheric and coronal abundances.

  10. The ambient Mg abundance relative to O for twelve SMM flares. The average ratio appears to be somewhat above photospheric values but is not consistent with that found in the corona.

  11. The ambient Si abundance relative to O for twelve SMM flares. The average ratio is close to the coronal value. It is important to note that the line is near the instrumental backscatter peak of the neutron- capture line.

  12. The ambient Fe abundance relative to O for twelve SMM flares. The average ratio appears to be consistent with photospheric values and is not consistent with that found in the corona. There is therefore no consistent evidence for a FIP effect in the ambient medium where the ions interact.

  13. Results of our fits on the 1989 October 19 flare at heliocentric of 30o. The He/O ratio (dotted curves) consistent with the Asplund et al. photospheric abundance is consistent with the chi2 contours from our fits. The accelerated ion spectrum is consistent with a power law with index between ~3.2 and 4.2.

  14. We obtained the accelerated abundances relative O for the 88 December 16 flare; the uncertainties are larger than for the ambient abundances. C/O is consistent with the Anders and Grevesse photospheric value; the heavy nuclei (Ne, Mg, Si, and Fe) also have a combined abundance consistent with what is found in the photosphere. It appears to be inconsistent with impulsive SEPs.

  15. The accelerated C abundance relative to O for twelve SMM flares. The average ratio appears to be consistent with all but Asplund et al. photospheric abundances.

  16. The accelerated heavy (combined Ne, Mg, Si, S, and Fe abundance normalized to Fe) relative to O for twelve SMM flares. The average ratio appears to be consistent with photospheric values but not with the strong enhancement found in impulsive SEP events.

  17. We have roughly estimated the accelerated alpha/proton ratios for the 12 flares from using acceptable ranges of He/O from Asplund. The average ratio is 0.15 and shows weak evidence for possible flare-flare variability

  18. Current Status of our Studies Fit 12 SMM spectra with bremsstrahlung, 0.511/2.2 MeV lines, and nuclear templates developed from empirical measurements and TALYS using a new instrument response. Abundances determined from Asplund He/O. Average ambient C/O abundance ratio appears to be in better agreement with Anders and Grevesse and coronal (gradual SEP) abundances than the Asplund et al. abundances. Average ambient Mg and Fe abundance ratio consistent with photospheric abundances while ambient Si abundance appears to be closer to coronal. No consistent low FIP enhancement. The average Ne/O abundance in the lower chromosphere has been measured directly for the first time with a value of 0.15-0.20. Average accelerated C/O abundance ratio consistent with coronal and Anders and Grevesse abundances but not Asplund et al. Average accelerated heavy ion (Ne, Mg, Si, and Fe)/O abundance ratio consistent with corona and photosphere but not impulsive SEPs. The average accelerated alpha/proton ratio (~0.15 ) is elevated.

  19. Measured Compton Scattered 2.2 MeV Line at the Sun from 1989 October 19 Flare Scattered Flux (>300 keV)/2.223 MeV Line Flux = 0.9 +- 0.1 Calculated ratio for the continuum >200 keV ~1.2 This is the first measurement of the 2.223 MeV Compton scattered flux. Other well-measured flares give similar ratios.

  20. Inferred Electron Spectra Best fitting bremsstrahlung photon spectra with uncertainties shown by the thin solid (blue lines). The spectrum hardens significantly above a few hundred keV and then appears to role over. Using SSW (Holman code) we fit the spectra by eye assuming that the electron spectrum is a sum of two power laws: a steep PL (dots) and a very hard PL which breaks at high energy (dashes). The combined fit is shown by the bold curve.

  21. Estimated Spectral Parameters for the Accelerated Electron Spectra 1981 April 27 1989 October 19 PL Index 1 ~4.6 ~5.4 e/sec (>100 keV) ~5 x 1033 ~1.5 x 1034 PL Index 2 ~1.1 ~1.05 Break Energy ~10 MeV ~22 MeV H.E. Index ~5.5 ~10 e/sec (>100 keV) ~2.8 x 1029 ~1.5 x 1029 Energy in electrons ~2.1 x 1030 erg ~1 x 1031 erg (>100 keV) Energy in ions ~6 x 1030 erg ~1 x 1031 erg (>1 MeV) NC/NP ~6 x 10-4 ~8 x 10-4 Solar atmosphere ~2-4 x 10-4 Proton Spectral index 3.2-4.3 3.7 – 5.0

  22. Flare gamma-ray spectrum revealing the different components that provide information on the accelerated-particle population and ambient material Cartoon illustrating particle acceleration and transport near the Sun.

  23. Lines and continua from p and alpha interactions

  24. Fits to the 1981 April 27 flare showing the total fit, bremsstrahlung, direct interaction (i.e. accelerated p and a on ambient elements), inverse interaction (i.e. heavy ions on ambient elements), a-4He, and 0.511/2.223 MeV line components and Compton-scattered 2.2 MeV line.

  25. Toner and MacKinnon (2004) have suggested that accelerated proton and alpha particles have different spectral indices. Such a harder spectrum may explain the strong -He line complex and yet yield ambient He/O ratios found in the photosphere. Preliminary studies suggest no significant improvement but studies are in progress.

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