By Vik Dhillon (auth.), A. Evans, Janet H. Wood (eds.)
In 1993 we started to give some thought to the potential for retaining a convention on Catacysmic Variables (CVs) at Keele college. there were a number of conferences within the region of CVs lately (e. g. Eilat, Abano-Padova, Capetown). in spite of the fact that as arrangements for the Keele assembly improved we discovered that, whereas there have been a couple of IAU conferences dedicated to comparable and to peripheral issues (such as IAU Colloquium 122 on Classical Novae in 1989, IAU Colloquium 129 on Accretion Disks in 1990), there have been no IAU-sponsored meetings within the zone of cataclysmi/: variables (CVs) for a few years. We felt hence that the time used to be ripe to have an IAU assembly de voted to an summary of CVs and similar gadgets and the SOC geared up the convention such that there has been an emphasis on invited reports of the latest advances within the box. The convention coated either CVs and LMXBs and the inter-relations among them. The assembly used to be held at a time while robust satellite tv for pc observatories, and speedy advancements in flooring established instrumentation, had ended in many advances in either CV and LMXB examine. The convention supplied a discussion board to study observations from ASCA, EUVE, ROSAT, Ginga and the recently-refurbished HST. picture metric, spectroscopic and polarimetric observations of CVs and LMXBs have thrown new mild at the distribution of topic and the character of the stellar parts in those systems.
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Additional info for Cataclysmic Variables and Related Objects: Proceedings of the 158th Colloquium of the International Astronomical Union, Held at Keele, United Kingdom, June 26–30, 1995
This has tended to favour the more luminous members (Mv '" 7 ... 10 mag) lying nearby in the Galactic plane (z < 400pc). In order to alleviate this bias, Howell & Szkody (1990) compiled a list of ",90 CV s that were faint enough and were at high galactic latitude to potentially place them well outside the Galactic plane, in the halo. We have obtained infrared J and K band images of a number of the CVs listed by Howell & Szkody (1990) in order to establish whether these systems are truely at large distances, or are instead a population of intrinsically faint objects lying relatively nearby.
WADE 6 , 1. Space Telescope Science Institute, USA 2. University of St. Andrews, Scotland, UK 3. Goddard Space Flight Center, USA 4. Lawrence Livermore Nat. , USA 5. Royal Greenwich Observatory, Teneri[e, Canary Islands 6. Pennsylvania State University, USA Abstract. We report first results of the HST /FOS time-resolved, lowresolution spectroscopy of the eclipsing cataclysmic variable UX UMa, including multi-wavelength mapping of its accretion disk in the ultraviolet region. 1. Introduction The Faint Object Spectrograph on HST was used to monitor the nova-like UX UMa during eclipse.
M. RUTTEN 5 , R. A. WADE 6 , 1. Space Telescope Science Institute, USA 2. University of St. Andrews, Scotland, UK 3. Goddard Space Flight Center, USA 4. Lawrence Livermore Nat. , USA 5. Royal Greenwich Observatory, Teneri[e, Canary Islands 6. Pennsylvania State University, USA Abstract. We report first results of the HST /FOS time-resolved, lowresolution spectroscopy of the eclipsing cataclysmic variable UX UMa, including multi-wavelength mapping of its accretion disk in the ultraviolet region.
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