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Observations of X-Ray Jets Using Yohkoh Soft X-Ray Telescope

  • K. Shibata (a1), Y. Ishido (a2), L. Acton (a3), K. Strong (a3), T. Hirayama (a1), Y. Uchida (a4), A. Mcallister (a4), R. Matsumoto (a5), S. Tsuneta (a6), T. Shimizu (a6), H. Hara (a6), T. Sakurai (a1), K. Ichimoto (a1), Y. Nishino (a1) and Y. Ogawara (a7)...

Abstract

Time series of SXT (Soft X-ray Telescope) images have revealed many jet-like features in the solar corona. Typical size of the “jet” is 5 × 103 – 4 × 105 km, the typical projected velocity is 30 – 300 km/s, and the kinetic energy estimated to be 1025 – 1028 erg. Many of the jets are associated with flare-like bright points or sub-flares. Three typical examples are discussed, including an X-ray jet identified with an Hα surge. It is suggested that magnetic reconnection is one of the possible mechanisms to produce these X-ray jets.

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Copyright

References

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Hara, H. et al.: 1992, Publ. Astron. Soc. Japan, 44, in press
Hirayama, T.: 1974, Solar Phys., 34, 323
Sakurai, T. et al: 1992, Publ. Astron. Soc. Japan, 44, L7
Shibata, K. and Uchida, Y.: 1986, Solar Phys., 103, 299
Shibata, K., Nozawa, S., and Matsumoto, R.: 1992a, Publ. Astron. Soc. Japan, 44, 265
Shibata, K., Nozawa, S., and Matsumoto, R.: 1993, in these proceedings
Shibata, K. et al.: 1992b, Publ. Astron. Soc. Japan, 44, in press.
Sterling, A. C., Shibata, K., and Mariska, J.T.: 1993, Astrophys. J., in press.
Tsuneta, S. et al.: 1991, Solar Phys., 136, 37.

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