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Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 1 A. Evans,Janet H. Wood Conference proceedings 1996 Kluwer Academic Publishe

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書(shū)目名稱(chēng)Cataclysmic Variables and Related Objects
副標(biāo)題Proceedings of the 1
編輯A. Evans,Janet H. Wood
視頻videohttp://file.papertrans.cn/223/222414/222414.mp4
叢書(shū)名稱(chēng)Astrophysics and Space Science Library
圖書(shū)封面Titlebook: Cataclysmic Variables and Related Objects; Proceedings of the 1 A. Evans,Janet H. Wood Conference proceedings 1996 Kluwer Academic Publishe
描述In 1993 we began to consider the possibility of holding a conference on Catacysmic Variables (CVs) at Keele University. There have been several meetings in the area of CVs recently (e. g. Eilat, Abano-Padova, Capetown). However as preparations for the Keele meeting progressed we realized that, while there had been a number of IAU meetings devoted to related and to peripheral topics (such as IAU Colloquium 122 on Classical Novae in 1989, IAU Colloquium 129 on Accretion Disks in 1990), there had been no IAU-sponsored conferences in the area of cataclysmi/: variables (CVs) for a number of years. We felt therefore that the time was ripe to have an IAU meeting de- voted to an overview of CVs and related objects and the SOC organized the conference such that there was an emphasis on invited reviews of the most recent advances in the field. The conference covered both CVs and LMXBs and the inter-relations between them. The meeting was held at a time when powerful satellite observatories, and rapid improvements in ground based instrumentation, had led to many advances in both CV and LMXB research. The conference provided a forum to review observations from ASCA, EUVE, ROSAT, Ginga and the
出版日期Conference proceedings 1996
關(guān)鍵詞Accretion; Common Envelope; Supernova; stars
版次1
doihttps://doi.org/10.1007/978-94-009-0325-8
isbn_softcover978-94-010-6632-7
isbn_ebook978-94-009-0325-8Series ISSN 0067-0057 Series E-ISSN 2214-7985
issn_series 0067-0057
copyrightKluwer Academic Publishers 1996
The information of publication is updating

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發(fā)表于 2025-3-21 23:24:58 | 只看該作者
The Nova-Likes Ac Cnc, Rw Tri, Ux Uma and the Nova Dq Her: Common and Different Propertiesysis is based on simultaneous high-speed UBVRI photometry, covering several dozens of orbital cycles evenly distributed over 14 years (1982...1995) for DQ Her, and over 11 years (1985...1995) for the other three stars. All data have been obtained with the 1.25 m telescope at the Crimean Astrophysica
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發(fā)表于 2025-3-22 01:47:53 | 只看該作者
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發(fā)表于 2025-3-22 08:00:14 | 只看該作者
Applications of Indirect Accretion Disc Imaging to Orbital Solutions for Primary Stars is a problem for which there is no universally applicable solution. Velocity measurements are handicapped because the accretion disc about the primary often dominates the optical spectrum. Therefore spectroscopists resort to measuring line profile symmetry in individual spectra of the accretion dis
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發(fā)表于 2025-3-22 10:25:52 | 只看該作者
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發(fā)表于 2025-3-22 15:45:54 | 只看該作者
Studies in Flickering bother studying this ‘noise’? Three reasons come to mind: (i) flickering is a fundamental signature of accretion, to the point of being a necessary characteristic (if it doesn’t flicker, it’s not a CV); (ii) energetically, flickering is not a small effect and can contribute up to a few tens of perc
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發(fā)表于 2025-3-22 17:55:45 | 只看該作者
Decomposing Interacting Binary Light Curves: The Eclipses of the Mean Light, Secular Variability andnes the orbital dependence (including eclipses) of the mean light, secular variability and RMS flickering. We identify the true line of centres of RW Tri and find that the accretion disc is a location of secular variability and a source of flickering.
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發(fā)表于 2025-3-22 23:08:23 | 只看該作者
The Place of Origin of the Flickering in Z Cha(iv) scintillation (negligible) and (v) any residual noise. Calculating the rms-scatter of the count rates in a light curve as a function of orbital phase, ?, through accretion disk eclipse of high inclination CVs — after subtraction of a smoothed light curve to remove orbital and long-term variatio
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發(fā)表于 2025-3-23 02:50:25 | 只看該作者
TT Ari-94: A Study of 1.6...60 Minute Variabilityy range 10...900 cycle d. are found. The highest peaks in the power spectrum cover the wide range of 28...139 cycle d.. Variations occur at a few preferred time-scales rather than at one cycle length, with a possible secular decrease. In the frequency range 90...900 cycle d. the power spectrum obeys
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發(fā)表于 2025-3-23 09:06:31 | 只看該作者
Time Resolved Optical Spectroscopy of V795 Herurce is examined using two-dimensional image analysis and Doppler reconstruction techniques on the orbital profiles. A clear S-wave modulation of a weak emission feature in the H? and Hγ line wings (extending to ~1800kms.) is present, with complex asymmetric properties.
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