Abstract
The X-ray emission mechanism of OB stars is still an unresolved problem. One possible emission mechanism involves hot gases produced by periodic shocks ploughing through the wind (Lucy & White 1980; Lucy 1982). Coronal models are viable alternatives: A photoionized hot corona can explain the observed soft X-ray spectra of OB stars. In this case, however, the origin of the hot corona is a problem (Stewart & Fabian 1981; Waldron 1984). A crucial key point to distinguish the above two models might be high quality measurements of soft X-ray spectra in order to confirm emission lines and absorption edges. So far, some detections of line emission have been reported (Cassinelli & Swank 1983; Corcoran et al. 1994; Kitamoto & Mukai 1996). These emission lines definitely indicate that the X-ray emission is thermal. But still the origin of the high temperature plasma is an open problem. In this work, we report ASCA SIS (Tanaka, Inoue & Holt 1994) observation results of four 0 stars: ζ Ori, λ Ori, δ Ori and ζ Pup.
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© 1996 Kluwer Academic Publishers
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Kitamoto, S., Suzuki, T., Torii, K., Ohno, Y. (1996). X-Ray Emission from O-Stars. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_29
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DOI: https://doi.org/10.1007/978-94-009-0315-9_29
Publisher Name: Springer, Dordrecht
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