Hostname: page-component-76fb5796d-qxdb6 Total loading time: 0 Render date: 2024-04-26T21:33:32.178Z Has data issue: false hasContentIssue false

IV. Results from Hinotori and P78-1

Published online by Cambridge University Press:  25 April 2016

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Hinotori observed 720 flares through its operation February 1981-October 1981. General discussions of the results were given in two symposia: the Hinotori Symposium (ISAS 1982) and the U.S.-Japan Seminar (de Jager & Švestka 1983). The hard x-ray imaging made at the effective energy 20-35 keV showed a wide variety of morphology. Many flares (22 out of 30 events) showed single source structure, either compact (12) or extended (10) in the spatial resolution of 15 arc sec (Takakura et al. 1983a, Ohki et al. 1983, Takakura 1984). Evidences are given in some limb events that the main source is located in the high corona (1-4 x 104 km) (Takakura et al. 1983b). The extended single source could be the whole coronal loops which may include footpoints, but the maximum brightness is near the loop top. In some events (8 out of 30), weak subsource(s) which sould be identified with the footpoint(s) appear intermittently (Tsuneta et al. 1983). Takakura et al. (1984) found that the extended single source becomes compact and slightly shifts to higher altitudes in later phases of the impulsive burst (5 out of 10 events). Tanaka (1984), Takakura (1984), and Tanaka S Zirin (1984) argued that the hard x-ray morphology of the impulsive burst is consistent with the non-thermal electron beam model in high density corona. Sakurai (1983) investigated magnetic field structures of the hard x-ray sources based on the potential field calculations. Timing between the hard x-ray and microwave in the impulsive bursts was examined by Takakura et al. (1983c), who found correlated subsecond time structures and also by Takakura et al. (1983d), who found a long (5-10 s) delay of the peaks at 17 GHz and E > 300 keV to the peak at E < 100 keV. Kurokawa (1983) showed detailed coincidence between the hard x-ray spikes and Hα brightenings.

Type
Research Article
Copyright
Copyright © Reidel 1985

References

Akita, K., Tanaka, K., and Watanabe, T.: 1983, Solar Phys. 86(1/2), 101105.Google Scholar
Culhane, J.L., Gabriel, A.H., Acton, L.W., Rapley, C.G., Phillips, K.J.H.,Wolfson, C.J., Antonucci, E., Bentley, R.D., Catura, R.C., Jordan, C., Kayat, M.A., Kent, B.J., Leibacher, J.W., Parmar, A.N., Sherman, J.C., Springer, L.A., Strong, K.T., and Veck, N.J.: 1981, Astrophys. J. Letters 244, L141.Google Scholar
de Jager, C. and Švestka, Z. (eds.): 1983, “Recent Advances in the Understanding of Solar Flares,” Solar Phys. 86(1/2).Google Scholar
Doschek, G.A., Kreplin, R.W., and Feldman, U.: 1979, Astrophys. J. Letters 233, L157.Google Scholar
Doschek, G.A., Feldman, U., Kreplin, R.W., and Cohen, L.: 1980, Astrophys. J. 239, 725.Google Scholar
Doschek, G.A., Feldman, U., Landecker, P.B., and McKenzie, D.L.: 1981, Astrophys. J. 249, 372.Google Scholar
Feldman, U., Doschek, G.A., Kreplin, R.W., and Mariska, J.T.: 1980, Astrophys. J. 241, 1175.Google Scholar
Feldman, U., Doschek, G.A., and Kreplin, R.W.: 1982a, Astrophys. J. 260, 885.Google Scholar
Feldman, U., Cheng, C.C., and Doschek, G.A.: 1982b, Astrophys. J. 255, 320.Google Scholar
ISAS: 1982, Hinotori Symposium on Solar Flares, Institute of Space and Aeronautical Science, Tokyo, Japan.Google Scholar
Kai, K. et al.: 1985, Publ. Astron. Soc. Japan (in press).Google Scholar
Kawabata, K., Ogawa, H., and Suzuki, I.: 1983, Solar Phys. 86(1/2), 247252.Google Scholar
Krutov, V.V., Korneev, V.V., Mandelstam, S.L., Shlyaptseva, A.S., Urnov, A.M., Vinogradov, A.V., and Zhitnik, I.A.: 1981, Lebedev Physical Institute Preprint No. 133.Google Scholar
Kurokawa, H.: 1983, Solar Phys. 86(1/2), 195196.Google Scholar
Lin, R.P., Schwartz, R.A., Pelling, R.M., and Hurley, K.C.: 1981, Astrophys. J. Letters 251, L109.Google Scholar
McKenzie, D.L., Landecker, P.B., Broussard, R.M., Rugge, H.R., Young, R.M.,Feldman, U., and Doschek, G.A.: 1980, Astrophys. J. 241, 409.Google Scholar
McKenzie, D.L. and Landecker, P.B.: 1982a, Astrophys. J. 259, 372.Google Scholar
McKenzie, D.L. and Landecker, P.B.: 1982b, Astrophys. J., 254, 309.Google Scholar
Nitta, N., Takakura, T., Ohki, K., and Yashimori, M.: 1983, Solar Phys. 86(1/2), 241246.Google Scholar
Ohki, K., Takakura, T., Tsuneta, S., and Nitta, N.: 1983, Solar Phys. 86(1/2), 301312.Google Scholar
Sakurai, T.: 1983, Solar Phys. 86(1/2), 339344.Google Scholar
Takakura, T.: 1984, Int. Workshop on Solar Phys. and Interplanet. Travelling Phenom., Kunming, China, Acad. Sinica (in press).Google Scholar
Takakura, T., Ohki, K., Tsuneta, S., and Nitta, N.: 1983a, Solar Phys. 86(1/2), 323331.Google Scholar
Takakura, T., Tsuneta, S., Ohki, K., Nitta, N., Makishima, K., Murakami, T., Ogawara, Y., Oda, M., and Miyamoto, S.: 1983b, Astrophys. J. Letters 270, L83.Google Scholar
Takakura, T., Kaufmann, P., Costa, J.E.R., Deganokar, S.S., Ohki, K., and Nitta, N.: 1983c, Nature 302, 317.Google Scholar
Takakura, T., Degaonkar, S.S., Ohki, K., Kosugi, T., and Enome, S.: 1983d, Solar Phys. 89, 379390.Google Scholar
Takakura, T., Ohki, K., Nitta, N., and Wang, J.L.: 1984, Astrophys. J. Letters 281, L51.Google Scholar
Tanaka, K.: 1984, Activities in Red Dwarf Stars, Proc. IAU Colloquium 71, Catania, Italy, p. 307.Google Scholar
Tanaka, K. and Akita, A.: 1984, Astrophys. J. (submitted).Google Scholar
Tanaka, K. and Zirin, H.: 1984, Astrophys. J. (submitted).Google Scholar
Tanaka, K., Watanabe, T., Nishi, K., and Akita, K.: 1982a, Astrophys. J. Letters 254, L59.Google Scholar
Tanaka, K., Nitta, N., and Watanabe, T.: 1982b, in Hinotori Symp. on Solar Flares (ISAS: Tokyo, Japan), pp. 2023.Google Scholar
Tanaka, K., Akita, K., Watanabe, T., and Nishi, K.: 1982c, in Hinotori Symp. on Solar Flares (ISAS: Tokyo, Japan), pp. 4357.Google Scholar
Tanaka, K., Nitta, N., Akita, K., and Watanabe, T.: 1983, Solar Phys. 86(1/2), 91100.Google Scholar
Tanaka, K., Watanabe, T., and Nitta, N.: 1984, Astrophys. J. 282, 793.Google Scholar
Tsuneta, S.: 1984, Astrophys. J. (in press).Google Scholar
Tsuneta, S., Takakura, T., Nitta, N., Ohki, K., Makishima, K., Murakami, T., Oda, M., and Ogawara, Y.: 1983, Solar Phys. 86(1/2), 313321.Google Scholar
Tsuneta, S., Takakura, T., Nitta, N., Ohki, K., Tanaka, K., Makishima, K., Murakami, T., Oda, M., Ogawara, Y., and Kondo, I.: 1984a, Astrophys. J. 280, 887891.Google Scholar
Tsuneta, S., Nitta, N., Ohki, K., Takakura, T., Tanaka, K., Makishima, K., Murakami, T., Oda, M., and Ogawara, Y.: 1984b, Astrophys. J. 284, 827832.Google Scholar
Watanabe, T., Tanaka, K., Akita, K., and Nitta, N.: 1983, Solar Phys. 86(1/2), 107113.Google Scholar
Yoshimori, M., Okudaira, K., Hirasima, Y., and Kondo, I.: 1983, 18th Internat. Cosmic Ray Conf. Vol. 4, pp. 8588 (Tata Inst. Fundamental Res.: Bombay).Google Scholar