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Astron. Astrophys. 336, 960-965 (1998)

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4. Conclusions

V635 Cas is now classified as an O9e star. We have demonstrated that a true spectral classification, although difficult to obtain, is needed to accurately model the BeXRBs. The filling in of critical lines by the disk emission precludes a determination of the luminosity class. We hope that future observations during a disk-loss event will improve on this result.

The far red spectra are an ideal probe of the circumstellar disk. Higher resolution spectra including additional lines in the Paschen series would enable us to confirm various line blends/strengths and measure the peak separation between the wings in the individual lines. This would enable us to model the size, density and velocity distribution in the disk. In particular the line profiles would help us parameterize the tidal effects of the neutron star at periastron.

Clearly this is a complex system as demonstrated by the dramatic spectral and photometric changes that occur on a short timescale of [FORMULA]months. A precise determination of the spectral class, luminosity and vsini requires frequent high resolution simultaneous multi-wavelength observations in order to catch the system in a disk-less state. In particular infrared observations of the HI lines are needed to further constrain the disk models.

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© European Southern Observatory (ESO) 1998

Online publication: July 27, 1998
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