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ASCA Observations of 44I Bootis and VW Cephei

Published online by Cambridge University Press:  25 May 2016

Chul-Sung Choi  and
Tadayasu Dotani
Chul-Sung Choi
Affiliation:
Korea Astronomy Observatory, 36-1 Hwaam, Yusong, Taejon 305-348, Korea; cschoi@hanul.issa.re.kr
Tadayasu Dotani
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229, Japan; dotani@astro.isas.ac.jp

Abstract

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We analyze X-ray archive data of the W UMa-type binaries 44i Boo and VW Cep, taken with ASCA on 1994 May 10 and 1993 November 5, respectively. By analyzing the light curve of VW Cep, we find a long-duration flare of ≈ 7.5 hrs with the peak luminosity of 1.2 × 1030 ergs s−1 (0.4-3.0 keV) for the assumed distance of 23.2 pc. We also find appreciable flux variations from the light curve of 44i Boo, and the variations are erratic and are not orbital phase dependent. From the spectral analysis of both data, we see that the spectra could be reproduced by the variable abundance plasma model with a combination of two different temperatures, kT = 0.64 – 0.65 keV and kT = 1.85 – 1.91 keV.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 226 - 227
Copyright
Copyright © Kluwer 1998 

References

Choi, C. S., & Dotani, T. 1998, ApJ , 492, in press CrossRefGoogle Scholar
McGale, P. A., Pye, J. P., & Hodgkin, S. T. 1996, MNRAS , 280, 627 Google Scholar
Pallavicini, R., Tagliaferri, G., & Stella, L. 1990, A&A , 228, 403 Google Scholar
Vilhu, O., Caillault, J.-P., & Heise, J. 1988, ApJ , 330, 922 CrossRefGoogle Scholar