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

By Alan H. Batten (auth.), Alan H. Batten (eds.)

When leaving the Victoria airport the day sooner than our Colloquium, I observed a van of the Dunsmuir inn marked with large letters which I learn as "Alcohol Colloquium". I do usually make such errors as a result worldwide, informal, and careless means during which I learn a variety of advertisements, and checked myself speedy to learn it properly as "Algol Colloquium". thousands of fellow voters may perhaps simply make an analogous mistake, and no apology might be anticipated. Even I learn and listen to the note alcohol extra usually than Algol, even if i have to say that Algols have given me extra excitement and less complications through the years; in that, besides the fact that, i could be a singularity, and doubtless a pitiful one at that. Being appointed Chairman of the clinical Organizing Committee, i'll be deemed to be a purer" Algolist" than different investigators, even though my variety of energetic pursuits is far broader; and an analogous is correct approximately the entire 28 invited audio system and all of the different members of the Colloquium. Our curiosity are strongly diverse, yet there are numerous strong purposes that introduced us jointly at this Colloquium.

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Read or Download Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988 PDF

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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

Example text

Following procedures used with RZ Oph (Olson 1987), the ratio of disk to cool-star light in primary eclipse totality was derived, and is in PHOTOMETRIC EFFECfS OF ACCRETION DISKS 25 complete agreement with Popper's spectroscopic results, noted earlier. That is, non-stellar light dominates the cool-star light in totality shortward of about 4000 A. Photometric signature 1, abnormal dips bordering primary eclipse, are clearly evident in Fig. 2. Because light curves are particularly unstable between secondary and primary eclipse, only the dip following eclipse was used to determine the disk emission.

And Stoehr, C. A. (1986). Astron. J. 91, 1418. Persson, S. E. (1988). Pub1. Astron. Soc. Pacific 100, 710. Peters, G. J. (1980), in Close Binary Stars ~ Observation and Interpretation, ed. M. J. P1avec, D. M. 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.

For systems that fall in the middle of the r-q diagram, between the curves for wd and wmin' the behavior of the disk probably depends critically on the width of the gas stream relative to the primary (~Tl/2p). Systems with wider, less focused gas streams should display more variable Ha emitting regions. Differences in stream width and possible errors in systemic parameters may explain why the disks in SW Cyg and AD Her are less variable than the one in UX Mon, even though all three systems occupy the middle domain in the r-q diagram.

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