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 ahead of our Colloquium, I observed a van of the Dunsmuir inn marked with gigantic letters which I learn as "Alcohol Colloquium". I do frequently make such errors end result of the international, informal, and careless means within which I learn quite a few advertisements, and checked myself fast to learn it adequately as "Algol Colloquium". thousands of fellow electorate may simply make an analogous mistake, and no apology should be anticipated. Even I learn and listen to the notice alcohol extra often than Algol, even if 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'll 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 if my variety of energetic pursuits is far broader; and a similar is correct approximately all of the 28 invited audio system and the entire different contributors of the Colloquium. Our curiosity are strongly varied, yet there are numerous reliable 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

Sample text

Since the fractional radius of the primary scales as p-2/3, the shorter period systems tend to be located in the upper third of the diagram and the longer period systems in the lower third. Thus one can now understand why, as mentioned in §l, the visibility of Balmer emission in Algols has historically been linked to the period of the system. Based upon the data used for this study, we have the following empirical results: a. 5 days, permanent Het emission is rarely observed. 6 days), which displays weak Het emission outside of eclipse.

OLSON that the hot star is responsible, and that the bright 'high' state results from elevated mass accretion by the gainer. The luminosity difference between high and low states is about one-third of the low-state luminosity. The peak incremental accretion rate onto a synchronously rotating gainer is ~ 4xlO- 7 solar masses per year. If the hot star rotates super-synchronously, as seems likely, then the rate is correspondingly higher. 5. The dashed line is a light curve synthesized with the Wilson-Devinney program assuming only stellar light, and using the radii and inclination of Knee et al.

Infrared observations of RZ Oph, mainly outside primary stellar eclipse. The dashed line is a predicted light curve, assuming only stellar light in the system. Open circles are predictions of a dusty disk model (see text). 0 L -_ _ _ _ _ _ _~ u v b y Wavelength Fig. 6. text). 4 , - - - , - - - , - - - , . - - - - , . - - - - , . 2 .. J -100 -80 -60 -40 -20 o 20 Cycle Count E Fig. 7. Observed - calculated times of minima of RZ Oph. from the new linear ephemeris. 34 EDWARD C. OLSON DISCUSSION Rucinski emphasized the size of the dusty disks postulated for the systems of KU Cyg and RZ Oph.

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