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Titlebook: Novae and Related Stars; Proceedings of an In M. Friedjung Conference proceedings 1977 D. Reidel Publishing Company, Dordrecht, Holland 197

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發(fā)表于 2025-3-21 16:34:31 | 只看該作者 |倒序瀏覽 |閱讀模式
書目名稱Novae and Related Stars
副標題Proceedings of an In
編輯M. Friedjung
視頻videohttp://file.papertrans.cn/669/668331/668331.mp4
叢書名稱Astrophysics and Space Science Library
圖書封面Titlebook: Novae and Related Stars; Proceedings of an In M. Friedjung Conference proceedings 1977 D. Reidel Publishing Company, Dordrecht, Holland 197
描述Michael Friedjung Though known since antiquity, novae are still poorly under- stood and present many problems. There has tended to be a lack of communication between theoreticians and observers and between different schools of thought, in spite of the advances of recent years in certain directions (observations of ordinary novae at minimum and of dwarf novae, theory of the causes of the explosion, etc ??? ). The meeting whose proceedings are contained in this volume was organized to stimulate a confron- tation between the different ideas and results. The subject has changed a lot since 1963, when the previous international meeting was held. There were 61 participants at the conference from 17 countries, so very many groups ~oing research in the field of novae were represented. The reader will see that the subject has become more physical (we know for instance that the binary nature of novae is essential) but much work remains to be done. There is still a large gulf between theory and observation. May he find here many new ideas for future research! I would like to thank the French Centre National de la Recherche Scientifique for providing financial help. I must also thank the other
出版日期Conference proceedings 1977
關鍵詞Accretion; LOPES; accretion disk; photometry; spectroscopy; stars; stellar; telescope
版次1
doihttps://doi.org/10.1007/978-94-010-1217-1
isbn_softcover978-94-010-1219-5
isbn_ebook978-94-010-1217-1Series ISSN 0067-0057 Series E-ISSN 2214-7985
issn_series 0067-0057
copyrightD. Reidel Publishing Company, Dordrecht, Holland 1977
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沙發(fā)
發(fā)表于 2025-3-21 21:51:36 | 只看該作者
0067-0057 of communication between theoreticians and observers and between different schools of thought, in spite of the advances of recent years in certain directions (observations of ordinary novae at minimum and of dwarf novae, theory of the causes of the explosion, etc ??? ). The meeting whose proceeding
板凳
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地板
發(fā)表于 2025-3-22 06:59:12 | 只看該作者
Physical Parameters of Prenovae and Outburst Amplitudesres and white dwarf densities are, however, mutually exclusive over a wide range of M.. Only two novae, CP Pup and V1500 Cyg, have, under the assumption of O-type temperatures, densities within the white dwarf range and even they are found near the low-density limit. This leaves three explanations for minimum light:
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發(fā)表于 2025-3-22 12:33:00 | 只看該作者
Past and Future Novaes (NZ,), and dwarf novae, including U Geminorum stars (UG) and Z Camelopardalis stars (Z Cam). We exclude supernovae from the present discussion, and summarize the content and interrelationships of the other classes.
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發(fā)表于 2025-3-22 23:34:53 | 只看該作者
The Expansion of Novae before Light Maximum and the Formation of the Principal Envelopeed from the moment of explosion of a Nova up to the moment of appearance of the principal spectrum of the star. At first we should mention that already for three Novae we have information on their spectra, obtained before the explosion by means of objective prisms, see discussion of this in paper of Arhipova and Mustel (1975).
9#
發(fā)表于 2025-3-23 02:12:25 | 只看該作者
The Binary Nature of the Nova-Like Variable CD -42° 14462 velocity and intensity of these emissions indicates a hot spot on the following side of the accretion disk. Simultaneous rapid photometry reveals the flickering is not modulated with the orbital period, suggesting the inclination is too low for an eclipse or occultation of the hot spot.
10#
發(fā)表于 2025-3-23 06:08:17 | 只看該作者
Model of Nova Envelopesculations (Starrfield, Sparks, and Truran 1974), and by an analytical study (Nariai 1974). The latter predicts the increase in Te and almost constant L for the quasi-static envelope for a period of 0.5 . where ..
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