By Vik Dhillon (auth.), A. Evans, Janet H. Wood (eds.)
In 1993 we started to reflect on the potential of conserving a convention on Catacysmic Variables (CVs) at Keele collage. there were a number of conferences within the sector of CVs lately (e. g. Eilat, Abano-Padova, Capetown). even if as arrangements for the Keele assembly improved we learned that, whereas there were a couple of IAU conferences dedicated to similar and to peripheral themes (such as IAU Colloquium 122 on Classical Novae in 1989, IAU Colloquium 129 on Accretion Disks in 1990), there were no IAU-sponsored meetings within the region of cataclysmi/: variables (CVs) for a few years. We felt accordingly that the time used to be ripe to have an IAU assembly de voted to an outline of CVs and similar gadgets and the SOC equipped the convention such that there has been an emphasis on invited studies of the latest advances within the box. The convention coated either CVs and LMXBs and the inter-relations among them. The assembly was once held at a time whilst robust satellite tv for pc observatories, and swift advancements in floor established instrumentation, had ended in many advances in either CV and LMXB study. The convention supplied a discussion board to check observations from ASCA, EUVE, ROSAT, Ginga and the recently-refurbished HST. photograph metric, spectroscopic and polarimetric observations of CVs and LMXBs have thrown new gentle at the distribution of topic and the character of the stellar elements in those systems.
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Extra resources 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
Andrews, Fife KY169SS, UK 2. Astronomy Centre, University of Sussex, Falmer, Brighton BN19QH, UK The general inability of optical observations of low mass interacting binaries to provide accurate radial velocity measures for the stellar components is a problem for which there is no universally applicable solution. Velocity measurements are handicapped because the accretion disc about the primary often dominates the optical spectrum. Therefore spectroscopists resort to measuring line profile symmetry in individual spectra of the accretion disc in order to provide information on the primary's motion.
ANDRONOV ET AL. e. much below the error estimate. The values for B, V obtained quasi-simultaneously at JD 63 are very close, similar to the results of the UBVRI photometry by Efimov et al. (1995). The periodograms often show a few peaks of comparable height, arguing for a set of preferred time-scales, rather than a secular decrease like the change from 27 min 1962 to 17 m in 1985 suggested by Semeniuk et al. (1987). Characteristics of the highest peaks for 45 runs obtained in 1988 are presented by Tremko et al.
Our algorithm provides K = 97 ± 31 km s-l, suggesting that the previous determination was biased. More significantly, the phasing has been redetermined (dashed line, Fig. 2), providing a more canonical location for the bright spot emission. DISTANCES AND ABSOLUTE MAGNITUDES OF A SAMPLE OF FAINT CATACLYSMIC VARIABLES L. N. SPROATSl, S. B. HOWELL2, K. O. MASON 1 1. Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, England 2. Astrophysics Group, Planetary Science Institute, 620 N.
Cataclysmic Variables and Related Objects: Proceedings of the 158th Colloquium of the International Astronomical Union, Held at Keele, United Kingdom, June 26–30, 1995 by Vik Dhillon (auth.), A. Evans, Janet H. Wood (eds.)