Algols: Proceedings of the 107th Colloquium of the by Alan H. Batten (auth.), Alan H. Batten (eds.)

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 hotel marked with great letters which I learn as "Alcohol Colloquium". I do frequently make such errors as a result worldwide, informal, and careless manner during which I learn quite a few advertisements, and checked myself fast to learn it properly as "Algol Colloquium". thousands of fellow voters may simply make a similar mistake, and no apology may be anticipated. Even I learn and listen to the be aware alcohol extra often than Algol, even supposing i have 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 energetic pursuits is far broader; and an analogous is right approximately the entire 28 invited audio system and all of the different contributors of the Colloquium. Our curiosity are strongly assorted, yet there are a number of strong purposes that introduced us jointly at this Colloquium.

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Additional resources for Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988

Sample text

Frequently increased shell absorption, which may arise in a density enhancement in the inner accretion disk between the two stars, is seen THE Ha EMITTING REGIONS OF THE ACCRETION DISKS IN ALGOLS 21 before and after eclipse. Such a build-up of material could result from an interaction between the gas stream and disk. Observational errors in Rp and q and varying stream widths are possible reasons why the disks observed in some systems may differ from what is predicted. An unexpected Ha profile might be a clue that the systemic parameters are in need of improvement.

Popper, and R. K. Ulrich, p 287. Plavec, M. (1988). Astron. J. ~, 755. , Dobias, J. , Etzel, P. , and Weiland, J. E. (1984), in Future of Ultraviolet Astronomy Based on Six Years of IUE Research, p 240. Po1idan, R. S. (1987). Bull. Amer. Astron. Soc. 19, 709. Popper, D. M. (1964). Astrophys. J. 139, 143. Popper, D. M. (1965). Astrophys. J. 141, 314. Pringle, J. E. (1981). Annu. Rev. Astron. 19, 137. Shakura, N. , and Sunyaev, R. A. (1973). Astron. Astrophys. 24, 337. Shao, C-Y (1967). Astron. 72, 480.

The author thanks the faculty and staff of the UCLA Astronomy Department, and especially Drs. Mirek Plavec and Dan Popper, for hospitality and much assistance during a sabbatical leave when a first draft of this paper was written. Much helpful advice was provided as well by Drs. Dick Crawford, Paul Etzel, Mario Livio, Norm Markworth, Gerry Peters, Ron Polidan, Jim Pringle, Joe Smak, Brian Warner, Ron Webbink, Bob Wilson, and Art Young. San Diego State University observers were Clayton Heller, Jeff Hickey, Linda Humes, Karen Kramer, Vickie Paylor, Tom Santrizos, Juan Tamez, Scott Temple, and Mark Whittaker.

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