Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.322..631r&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 322, Issue 3, pp. 631-642.
Astronomy and Astrophysics
Astronomy
10
Binaries: Close, Stars: Individual: Qs Tel, Novae, Cataclysmic Variables, Ultraviolet: Stars, X-Rays: Stars
Scientific paper
Multiwavelength monitoring observations of the AM Her system, QS Tel, are presented, the centrepiece being a coordinated campaign with the ASCA, EUVE and HST satellites and optical observations on 1996 September 28-29. The star was initially observed in an intermediate brightness, single pole state in 1996 April by ROSAT. However two EUVE snapshots of the system in August found it in a deep low state, the light curves appearing to retain a bright and faint phase morphology although the bright interval showed significant phase drifts compared with the earlier ROSAT data. At this time, the system appeared optically bright, while polarimetry pointed to one active pole. A modest recovery of intensity, albeit accompanied by an apparently chaotic extreme ultraviolet (EUV) light curve, was subsequently recorded during the coordinated run in late September. This brightening was confirmed by a second ROSAT pointing in early October, although the EUV brightening is matched by a marked decay in its optical output. These observations, all of which found the system in a fainter EUV state than seen in 1993, add to the catalogue of accretion mode behaviour in QS Tel. However, as yet, the data base of observations does not allow us to establish whether the accretion mode is dictated by accretion-rate dependent penetration of the magnetosphere or asynchronous rotation. The ASCA spectrum obtained during the coordinated observation is adequately described by a thermal spectrum with a temperature of about 4.4keV and an absorbing column density of less than 8×1020cm-2. At the same time, the 1150-2600Å UV HST spectrum shows a strong, broad Lyα absorption profile which we attribute to the white dwarf. We infer an effective temperature of 16000-19000K and a mass between 0.5 and 0.93Msolar for the white dwarf, at least some of the uncertainty arising because the profile is very probably contaminated and broadened by Zeeman features. The orbital variation seen by HST can be matched by a blackbody-like spectrum with a temperature above 24000K. The near UV part of the spectrum contains evidence of phase-variable cyclotron harmonics.
Buckley David A. H.
Burleigh Matthew R.
de Martino Domitilla
Howell Steve B.
Lieu Richard
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