Titlebook: Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments; Proceedings of IAU C H. Drechsel,Y. Kondo,J. Rahe

amplitude

Fecal-Impaction

978-94-010-8191-7Springer Science+Business Media Dordrecht 1987

情節(jié)劇

Anjia Wang,Xinyao Yi,Yonghong Yanomponent. Mass exchange leads to cataclysmic events in such systems. The rate of semidetached low- mass close binary formation is 5xl0. yr. if the accreting component is a He degenerate dwarf, 5xl0. yr. if it is a CO-dwarf and 3x10. yr. if it is a neutron star. Systems with compact accretors arise a

STEER

厚顏

https://doi.org/10.1007/978-3-030-58144-2nt implications and clues about the nature and long-term evolution of cataclysmic variables can emerge from an analysis of their physical properties. Detection of the underlying white dwarfs has led to a preliminary empirical CV white dwarf temperature distribution function and, in a few cases, the

myalgia

Maximizer

https://doi.org/10.1007/978-3-030-58144-20–130 min) with those directly above (P=190– 240 min). Significant differences are found in the mean U-B,V-J colors and in the Hβ equivalent widths on the 2 sides of the gap. A detailed comparison from UV-IR of 3 high inclination novalike systems with periods near 3.3 hr (PG1012-029,PG1030+590 and V

無畏

Tiago H. Moreira de Oliveira,Marco Painholysmic variables have been identified and new observations of one already known object have been accumulated. Observations in the visible and UV-region show variability and differences in spectral type.If compared to the numbers of cataclysmic variables/white dwarfs as computed by Ritter and Burkert

headlong

https://doi.org/10.1007/978-3-030-58872-4he two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in t

嫻熟

Alexei Gvishiani,Anatoly Solovievclysmic system PHL 227 were determined from multi-wavelength spectroscopic and photometric data to search for general characteristics of these systems. The observed variations of the UV to IR spectral indices are qualitatively very similar for all systems, whereas the absolute values show significan