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

HARDY

書目名稱Novae and Related Stars影響因子(影響力)




書目名稱Novae and Related Stars影響因子(影響力)學(xué)科排名




書目名稱Novae and Related Stars網(wǎng)絡(luò)公開度




書目名稱Novae and Related Stars網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Novae and Related Stars被引頻次




書目名稱Novae and Related Stars被引頻次學(xué)科排名




書目名稱Novae and Related Stars年度引用




書目名稱Novae and Related Stars年度引用學(xué)科排名




書目名稱Novae and Related Stars讀者反饋




書目名稱Novae and Related Stars讀者反饋學(xué)科排名

效果

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

instulate

可忽略

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:

fledged

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.

intention

抱怨

叢林

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).

Meager

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.

凈禮

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 ..