Photoelectric observations of VW Cephei in R and I

Arai, K.

doi:10.1007/bf01583832

Cited by 1 publication

(1 citation statement)

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“…To determine the orbital phase of the dip, we use the ephemeris given in Aluigi et al (1994). Because the orbital period of VW Cep is known to change abruptly (Hill 1989;Arai 1994), it is essential to use the ephemeris determined with the closest data to the X-ray observation. We found that the mid-dip time corresponds to the orbital phase of 0.46.…”

Section: Data Analysis and Light Curvesmentioning

confidence: 99%

ASCAObservation of a Long‐Duration X‐Ray Flare from the W UMa–Type Binary VW Cephei

Choi

Dotani

1998

ApJ

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We analyze X-ray archive data of the W UMa-type binary VW Cep taken with ASCA on 1993 November 5 { 6. By analyzing the light curve, we nd a long-duration are of 7:5 hrs with the peak luminosity of 1:2 10 30 ergs s ?1 (0.4{3.0 keV) for the assumed distance of 23.2 pc. A ux dip is detected in the light curve at the orbital phase of 0:5, and it is identi ed as an eclipse by the secondary star. We determine the time scale of the eclipse egress to be 30 minutes from a model t to the light curve. With this time scale, we estimate the linear size of the aring region is 5:5 10 10 cm regardless of the are models. From the spectral analysis of the data, we nd that the spectrum can be well reproduced by the variable abundance plasma model with a combination of two di erent temperatures, kT = 0.64 keV and kT = 1.91 keV. The hotter component is considered to be associated with the are. The results are interpreted in terms of two-ribbon are model, in which we also discuss possible enhancement of element abundances.

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Section: Data Analysis and Light Curvesmentioning

confidence: 99%