Abstract
High-spectral-resolution measurements of the 2.223 MeV neutron capture line and the 0.511 MeV positron-electron annihilation line have been made with the Reuven Ramaty High-Energy Solar Spectroscopic Imager during the X4.8 flare of 23 July 2002. We have tried to explain both the time histories of the 2.223 MeV line and the 0.511 MeV line, adopting a power-law spectrum of accelerated ions. The results show that with a power-law spectral index of 3.52, the calculational time histories can roughly reproduce the observations. An improved fit between the calculated 2.223 MeV line and the observed 2.223 MeV line can be achieved if we allow the spectrum of accelerated ions to vary with time.
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References
Gan, W. Q.: 1998, Astrophys. J. 496, 992.
Gan, W. Q. and Rieger, E.: 1999, Solar Phys. 186, 311.
Hua, X. M. and Lingenfelter, R. E.: 1987, Solar Phys. 107, 351.
Hurford, G. J. et al.: 2003, Astrophys. J. 595, L77.
Kosugi, T., Dennis, B. R., and Kai, K.: 1988, Astrophys. J. 324, 1118.
Kozlovsky, B., Lingenfelter, R. E., and Ramaty, R.: 1987, Astrophys. J. 316, 801.
Lin, R. P., et al.: 2002, Solar Phys. 210, 3.
Lin, R. P., et al.: 2003, Astrophys. J. 595, L69.
Murphy, R. J., Dermer, C. D., and Ramaty, R.: 1987, Astrophys. J. Suppl. 63, 721.
Murphy, R. J. and Ramaty, R.: 1984, Adv. Space Res. 4(7), 127.
Murphy, R. J., Ramaty, R., Kozlovsky, B., and Reames, D. V.: 1991, Astrophys. J. 371, 793.
Murphy, R. J., Share, G. H., Letaw, J. R., and Forrest, D. J.: 1990, Astrophys. J. 358, 298.
Murphy, R. J. et al.: 2003, Astrophys. J. 595, L93.
Prince, T. A., Forrest, D. J., Chupp, E. L., Kanbach, G., and Share, G. H.: 1983, 18th ICRC 4, 79.
Ramaty, R.: 1986, in P. A. Sturrock, T. E. Holzer, D. M. Mihalas, and R. K. Ulrich (eds.), Physics of the Sun, Reidel Publishing Company, Dordrecht, Chapter 14.
Ramaty, R., Mandzhavidze, N., and Kozlovsky, B.: 1996, in R. Ramaty, N. Mandzhavidze, and X. M. Hua (eds.), AIP Conf. Proc., High Energy Solar Physics 374, 172.
Reames, D. V.: 1995, Adv. Space Res. 15(7), 41.
Schwartz, R. A., Csillaghy, A., Tolbert, A. K., Hurford, G. J., McTiernan, J., and Zarro, D.: 2002, Solar Phys. 210, 165.
Share, G. H. and Murphy, R. J.: 1997, Astrophys. J. 485 409.
Share, G. H., et al.: 2003, Astrophys. J. 595 L85.
Smith, D. M., et al.: 2002, Solar Phys. 210, 33.
Smith, D. M., et al.: 2003, Astrophys. J. 595, L81.
Trotett, G., et al.: 1993, Astron. Astrophys. Suppl. 97, 337.
Wang, H. T. and Ramaty, R.: 1974, Solar Phys. 36, 129.
Yoshimori, M., Shiozawa, A., and Suga, K.: 1999, 26th ICRC 6, 30.
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Gan, W. On Both the Time Histories of the 0.511 MeV Line and 2.223 MeV Line from the X4.8 Flare of 23 July 2002 Observed with Rhessi. Solar Physics 219, 279–287 (2004). https://doi.org/10.1023/B:SOLA.0000022961.17110.a4
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DOI: https://doi.org/10.1023/B:SOLA.0000022961.17110.a4