By Vik Dhillon (auth.), A. Evans, Janet H. Wood (eds.)
In 1993 we started to contemplate the opportunity of conserving a convention on Catacysmic Variables (CVs) at Keele collage. there were numerous conferences within the region of CVs lately (e. g. Eilat, Abano-Padova, Capetown). notwithstanding as arrangements for the Keele assembly stepped forward we discovered that, whereas there were a couple of IAU conferences dedicated to similar and to peripheral issues (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 quarter of cataclysmi/: variables (CVs) for a couple of years. We felt for that reason that the time was once ripe to have an IAU assembly de voted to an summary 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 lined either CVs and LMXBs and the inter-relations among them. The assembly used to be held at a time whilst strong satellite tv for pc observatories, and swift advancements in floor dependent instrumentation, had resulted in many advances in either CV and LMXB learn. The convention supplied a discussion board to study 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 subject and the character of the stellar parts in those systems.
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Additional 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
We estimate the FWHM of the 'narrow' absorption component in the Si IV doublet to be ",2000 km s-1. 0. 3. Discussion and conclusions Whilst the apparently different behaviour of V795 Her during these HST observations (d. our earlier IUE data) is perplexing, the orbitally related variability seen here does at least place the star -back amongst the more conventional wind-driving nova-like systems. However, two key new results emerge from these high quality data. Firstly, several lines show a 'narrow' absorption feature.
3 shows the so-called entropy landscape, which plots entropy as a function of masses of the primary and secondary star (see examples in Rutten & Dhillon 1994). 55M 0 . The radial velocities corresponding to this solution agree well with those measured from our data, as well as with published radial velocities. Note that Roche tomography automatically takes irradiation effects into account, and hence no a posteriori corrections are needed as in the case of masses determined from radial velocities only.
2. This map shows that the NaI line is less strong on the hemisphere facing the white dwarf. Presumably heating by irradiation causes a reduced line strength. So far, we have assumed that the binary star geometry is known. However, published binary star parameters are not in agreement over what the masses of the components are, which renders the results from Roche tomography less certain. To overcome this problem, rather than picking just one set of binary star masses, we reconstruct the Na I brightness map of the secondary star using a large number of combinations of masses, and from the set of solutions choose the one which, in line with the maximum entropy criterion, has the least structure.