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Flares and MHD Jets in Protostar

Published online by Cambridge University Press:  25 May 2016

Mitsuru Hayashi ,
Kazunari Shibata  and
Ryoji Matsumoto
Mitsuru Hayashi
Affiliation:
Japan Atomic Energy Research Institute(JAERI) 801-1 Mukouyama, Naka-machi, Naka-gun, Ibaraki, 311-01, Japan
Kazunari Shibata
Affiliation:
National Astronomical Observatory Mitaka, Tokyo 181, Japan
Ryoji Matsumoto
Affiliation:
Department of Physics, Faculty of Science, Chiba University Inage-Ku, Chiba 263, Japan

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By using ASCA, Koyama et al. (1994, 1996) carried out a systematic survey of hard X-ray sources in molecular clouds and revealed that protostars are strong hard X-ray emitting sources. Some of them show flare-like activities. Protostellar flares differ from solar flares in their total energy(1035-36 erg), size(several times the radius of protostar), and higher temperature(8keV). Protostellar flares are also observed in lower energy band by ROSAT in YLW15 (Grosso et al. 1997). By extending the model of solar flares associated with footpoint shearing motion, we proposed a model of protostellar flares in which the magnetic field connecting the protostar and the disk disrupt by twist injection from the rotating disk(Hayashi et al. 1996).

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 232 - 233
Copyright
Copyright © Kluwer 1998 

References

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