Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-27T04:35:00.197Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Published online by Cambridge University Press:  12 April 2016

K. Shibata ,
Y. Ishido ,
L. Acton ,
K. Strong ,
T. Hirayama ,
Y. Uchida ,
A. Mcallister ,
R. Matsumoto ,
S. Tsuneta  and
T. Shimizu
...Show all authors
K. Shibata
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
Y. Ishido
Affiliation:
STE Laboratory, Nagoya University, Toyokawa442
L. Acton
Affiliation:
Lockheed Palo Alto Research Laboratory, Palo Alto, U.S.A.
K. Strong
Affiliation:
Lockheed Palo Alto Research Laboratory, Palo Alto, U.S.A.
T. Hirayama
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
Y. Uchida
Affiliation:
Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo
A. Mcallister
Affiliation:
Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo
R. Matsumoto
Affiliation:
College of Arts and Sciences, Chiba University, Chiba260
S. Tsuneta
Affiliation:
Institute for Astronomy, The University of Tokyo, Mitaka, Tokyo181
T. Shimizu
Affiliation:
Institute for Astronomy, The University of Tokyo, Mitaka, Tokyo181
H. Hara
Affiliation:
Institute for Astronomy, The University of Tokyo, Mitaka, Tokyo181
T. Sakurai
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
K. Ichimoto
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
Y. Nishino
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
Y. Ogawara
Affiliation:
Institute of Space and Astronomical Science, Sagamihara229

Abstract

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.

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.

Type
Session 6. Flares and Transients
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 343 - 346
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

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