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ASCA Observations of Class I Protostars in the Rho Oph Dark Cloud

Published online by Cambridge University Press:  25 May 2016

Y. Tsuboi ,
K. Koyama ,
Y. Kamata  and
S. Yamauchi
Y. Tsuboi
Affiliation:
Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto, 606-01, Japan
K. Koyama
Affiliation:
Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto, 606-01, Japan
Y. Kamata
Affiliation:
Department of Astrophysics, School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-01, Japan
S. Yamauchi
Affiliation:
Faculty of Humanities and Social Sciences, Iwate University, 3-18-34, Ueda, Morioka, Iwate, 020, Japan

Extract

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On 1993 August 20, we observed the Rho-Oph dark cloud and detected hard X-rays from Class I sources (Koyama et al.(1994), Kamata et al.(1997)). One of the sources (EL29) showed a flare-like variability, while another (WL6) exhibited sinusoidal variation with no large spectral change. The later would be due to a spin of the protostar. The sinusoidal period of about 1 day is shorter than spin periods of TTSs of ~3-7 day.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 236 - 237
Copyright
Copyright © Kluwer 1998 

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