Abstract
We use the filter ratio method of analysis to determine spatially resolved values of plasma parameters in the X-ray emitting post-flare loop system which developed on 29 and 30 July 1973. We find that the loops were hotter and had higher plasma pressure at their tops than near their footpoints. The loop tops were at nearly the same temperature at different places 3 hr after the flare maximum and were also at nearly this same temperature 3 and 8 hr later. Variations in brightness transverse to the loops were due to variations in emission measure. We show by consideration of radiative losses alone that energy must have been added to the hottest part of the flare, at the tops of the loops, late into the decay phase of the flare.
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Cheng, C. C.: 1977, Solar Phys. 55, 413.
Dere, K. P., Horan, D. M., and Kreplin, R. W.: 1974, Solar Phys. 36, 459.
Dere, K. P., Horan, D. M., and Kreplin, R. W.: 1977, Astrophys. J. 217, 976.
Doschek, G. A., Feldman, U., and Rosenberg, F. D.: 1977, Astrophys. J. 215, 329.
Feldman, U., Doschek, G. A., and Rosenberg, F. D.: 1977, Astrophys. J. 215, 652.
Gerassimenko, M. and Nolte, J.: 1978, Solar Phys. 60, 299.
Kahler, S.: 1976, Solar Phys. 48, 255.
Kato, T.: 1976, Astrophys. J. Suppl. 30, 397.
Levine, R. H.: 1978, Solar Phys. 56, 185.
MacCombie, W. J. and Rust, D. M.: 1979, Solar Phys. 61, 69.
Martin, S. F.: 1979, Solar Phys. (in press, referred to as Paper III).
Nolte, J. T., Gerassimenko, M., Krieger, A. S., Petrasso, R. D., and Švestka, Z.: 1979 Solar Phys., this issue, p. 123 (referred to as Paper I).
Pallavicini, R., Vaiana, G. S., Kahler, S. W., and Krieger, A. S.: 1975, Solar Phys. 45, 411.
Pallavicini, R., Serio, S., and Vaiana, G. S.: 1977, Astrophys. J. 216, 108.
Raymond, J. C., Cox, D. P., and Smith, B. W.: 1976, Astrophys. J. 204, 290.
Rust, D. M.: 1976, Solar Phys. 47, 21.
Švestka, Z.: 1976, Solar Flares, D. Reidel Publ. Co., Dordrecht, Holland.
Švestka, Z., Dodson-Prince, H. W., Martin, S. F., Mohler, O. C., Moore, R. L., Nolte, J. T., and Petrasso, R. D.: 1979, to be submitted to Solar Phys. (referred to as Paper IV).
Tucker, W. H. and Koren, M.: 1971, Astrophys. J. 168, 283 (Erratum 170, 621).
Vaiana, G. S., Reidy, W. P., Zehnpfennig, T.; VanSpeybroeck, L., and Giacconi, R.: 1968, Science 161, 564.
Vaiana, G. S., VanSpeybroeck, L., Zombeck, M. V., Krieger, A. S., Silk, J. K., and Timothy, A.: 1977, Space Sci. Inst. 3, 19.
Vorpahl, J. A.: 1976, Astrophys. J. 205, 868.
Vorpahl, J. A., Tandberg-Hanssen, E., and Smith, J. B., Jr.: 1977, Astrophys. J. 212, 550.
Widing, K. G. and Cheng, C. C.: 1974, Astrophys. J. 194, L111.
Widing, K. G. and Dere, K. P.: 1977, Solar Phys. 55, 431.
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Petrasso, R.D., Nolte, J.T., Gerassimenko, M. et al. Study of the post-flare loops on 29 July 1973. Sol Phys 62, 133–144 (1979). https://doi.org/10.1007/BF00150140
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DOI: https://doi.org/10.1007/BF00150140