By Alan H. Batten (auth.), Alan H. Batten (eds.)
When leaving the Victoria airport the day earlier than our Colloquium, I observed a van of the Dunsmuir resort marked with giant letters which I learn as "Alcohol Colloquium". I do usually make such errors end result of the worldwide, informal, and careless means during which I learn a number of advertisements, and checked myself quick to learn it accurately as "Algol Colloquium". hundreds of thousands of fellow voters might simply make a similar mistake, and no apology may be anticipated. Even I learn and listen to the notice alcohol extra often than Algol, even supposing i need to say that Algols have given me extra excitement and less complications through the years; in that, even though, i could be a singularity, and doubtless a pitiful one at that. Being appointed Chairman of the clinical Organizing Committee, i could be deemed to be a purer" Algolist" than different investigators, even though my variety of lively pursuits is way broader; and a similar is correct approximately all of the 28 invited audio system and all of the different contributors of the Colloquium. Our curiosity are strongly diverse, yet there are numerous sturdy purposes that introduced us jointly at this Colloquium.
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Additional info for Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988
The star was observed at Villanova with H-alpha and H-beta filter sets and intermediate-band blue (A4530) and yellow (A5500) filters. BVRI filters were used with the APT. The comparison star was Gamma Lyr. The differential magnitudes for the H-alpha wideband filter are plotted against orbital phase in Fig. 3. These observations were obtained during 1970 to 1974 and different symbols are used for each observing season in the plot. As discussed earlier, this light curve and the others show large amounts of scatter.
CONCLUSIONS Some of the characteristics of the disks in selected Algol disks implied by this investigation are enumerated in Table 1. For each system, its period, phases at which disk occultation begin/ends (¢V, ¢R), the estimated radial extent of the disk relative to the size of the primary's Roche surface (Rd/~p), and comments on whether any asymmetry in brightness has been observed are given. The conclusions from this study can be summarized as follows: 1. The presence and stability of an Het emitting accretion disk appear to depend on the location of the system in the r-q diagram (Fig.
The disk emission is very red, and non-stellar. In connection with 'thick disks', it is relevant that P1avec (1988) had to invoke a thick, non-alpha, disk in his model of TT Hyd. There is a hint that the disk in RZ Oph may be slightly 'thick and dusty'. Shaviv and Wehrse (1986) suggest that disk thicknesses have been underestimated in classical alpha disks. We finally note that the slow brightness variations in KU Cyg are not present in primary eclipse totality, so the cool star cannot be their source (in agreement with Popper's conclusion).