By Alan H. Batten (auth.), Alan H. Batten (eds.)
When leaving the Victoria airport the day ahead of our Colloquium, I observed a van of the Dunsmuir resort marked with colossal letters which I learn as "Alcohol Colloquium". I do usually make such mistakes as a result of international, informal, and careless means within which I learn numerous advertisements, and checked myself quick to learn it properly as "Algol Colloquium". hundreds of thousands of fellow electorate may simply make an identical mistake, and no apology might be anticipated. Even I learn and listen to the note alcohol extra usually than Algol, even though i need to say that Algols have given me extra excitement and less complications through the years; in that, in spite of the fact that, i could be a singularity, and doubtless a pitiful one at that. Being appointed Chairman of the medical Organizing Committee, i could be deemed to be a purer" Algolist" than different investigators, even if my diversity of energetic pursuits is way broader; and an identical is right approximately the entire 28 invited audio system and the entire different contributors of the Colloquium. Our curiosity are strongly assorted, yet there are a number of stable purposes that introduced us jointly at this Colloquium.
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Extra resources for Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988
Period 40 EDW ARD F. GUINAN studies have been made from the 200 year data baseline which show that the orbital period is increasing with time at the rate of about 19 sec per year (Kreiner 1978). This large period increase has been -5 -6 interpreted as mass loss from the system at a rate of about 10 to 10 M@/yr. This high mass loss rate inferred from the eclipse timings is in accord with the spectroscopic studies of the system carried out at visual and ultraviolet wavelengths. As discussed by Sahade (1980), Beta Lyrae appears to reside inside a large, eKpanding envelope of hot turbulent gas.
I .... ~ WD 1 • ! 0 Orbital Phose Fig. 2. Infrared observations of KU Cyg, with the slow variation shifted out. 0, where the observer sees the region where stream and disk interact. These variations increase in size toward short wavelength. Open circles are predictions of a thick, dusty disk model (see text). , I. 7 ! o . -... . 0 I .. I ':tv:: . 6 :• J , , • . ' I, • 'i . \. 0 Orbital Phose Fig. 3. Shifted blue observations of KU Cyg. Secondary eclipse is shallower than it is at longer wavelengths.
Test calculations suggest- that the dip following primary eclipse will be nearly invisible if the mean disk temperature falls to about 4000 K. The leading half of the disk is therefore at least 1000 K hotter than the following half. Since the cool star fails to fill its Roche lobe (Olson and Hickey 1983; Knee et al. 1986), it is likely that the disk forms from a stellar wind. That wind is probably considerably amplified over the rate from a single star (Kenyon 1988). The hot gainer is carried by the relative stellar orbital motion into this wind at about 30 km/sec, a supersonic rate.
Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988 by Alan H. Batten (auth.), Alan H. Batten (eds.)