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Titlebook: Interacting Binaries; P. P. Eggleton,J. E. Pringle Book 1985 D. Reidel Publishing Company, Dordrecht, Holland 1985 accretion disk.astronom

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发表于 2025-3-21 16:39:47 | 显示全部楼层 |阅读模式
书目名称Interacting Binaries
编辑P. P. Eggleton,J. E. Pringle
视频video
丛书名称Nato Science Series C:
图书封面Titlebook: Interacting Binaries;  P. P. Eggleton,J. E. Pringle Book 1985 D. Reidel Publishing Company, Dordrecht, Holland 1985 accretion disk.astronom
描述Peter P. Eggleton and James E. Pringle Institute of Astronomy Madingley Road Cambridge England The 1970‘s can be described, in retrospect, as the "Decade of the Close Binary". Exciting observations with new technology, combined with classical work, both observational and theoretical, convinced the astronomical world that binary interaction of various kinds is not only interesting but common. Indeed, by 1975 almost anything unusual had a good chance of being interpreted as due to binary interaction. But astronomers are seldom overwhelmed by speculation, even their own, and solid observational work has confirmed or refuted such speculation, without regard to its plausibility. For instance, binarity has been found where it was perhaps least expected, in Barium stars, and refuted where it could most reasonably be expected, in Wolf-Rayets. Unfortunately, many other classes of potential binaries remain without the clearest evidence of binarity, for instance Be stars, symbiotics and blue stragglers. This Advanced Study Institute was held to commemorate John Whelan (1945-1981), whose scientific career, sadly cut short in its prime, did much to further the careful study, theoretical and obs
出版日期Book 1985
关键词accretion disk; astronomy; photometry; stellar; stellar evolution
版次1
doihttps://doi.org/10.1007/978-94-009-5337-6
isbn_softcover978-94-010-8856-5
isbn_ebook978-94-009-5337-6Series ISSN 1389-2185
issn_series 1389-2185
copyrightD. Reidel Publishing Company, Dordrecht, Holland 1985
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发表于 2025-3-21 22:02:37 | 显示全部楼层
Activity of Contact Binary Systems,nally called the “W UMa-type” systems. This limitation results mainly from a better knowledge of properties of cooler systems (i.e. with periods below about 0.5 – 0.6 days) but is also dictated by an expectation that only late-type stars can generate any magnetic activity.
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发表于 2025-3-22 07:55:12 | 显示全部楼层
Tidal Interactions of Close Binary Systems,mall orbital eccentricities (e.g. Young & Koniges 1977, Koch & Hrivnak 1981, Middelkoop & Zwaan 1982). There appears to be no such correlation for wide binary systems, which show a wide scatter of orbital eccentricities. This phenomenon is usually explained in terms of tidal interaction between the
发表于 2025-3-22 08:55:35 | 显示全部楼层
Wolf-Rayet Stars and Binarity,nformation on stellar masses, the motions and physics of interacting material streams connecting the stellar components and providing tests for binary stellar evolution models. The past decade has witnessed some significant changes to the picture of what constitutes a WR star and as to what role bin
发表于 2025-3-22 13:41:19 | 显示全部楼层
Photometry of Active Algols, and most notably in U Cep have these disturbances been large enough to analyse quantitatively. From a study of the spectral distribution of light excesses and losses in U Cep, we derive properties of “equatorial bulges,” hot spot, and stream during periods of activity presumably associated with tra
发表于 2025-3-22 17:32:20 | 显示全部楼层
From Algol to Beta Lyrae, be called .. β Lyrae is much more complicated, and some of the problems of revealing its structure are discussed. The best model available at the present considers β Lyrae as an Algol-type semi-detached system in a phase of fairly rapid mass transfer, i.e. younger than typical Algols. The most impo
发表于 2025-3-23 01:08:27 | 显示全部楼层
Symbiotic Stars,uch models leads to the conclusion that symbiotic stars are likely to be main sequence or white dwarf stars accreting material from a red (super)giant primary. Recent observations of symbiotic stars confirm this notion, and three systems (CI Cyg — a red giant with an accreting main sequence star com
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Optical Characteristics of X-Ray Binaries,ew years and has now reached about 100 (Bradt & McClintock 1983), mainly as a result of refined X-ray positions obtained with the Ariel 5, SAS-3 and HEAO-1 satellites. In these sources there are good reasons to believe that the X-ray emission results from accretion onto a collapsed object, matter be
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