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

想象

Alexei Gvishiani,Anatoly Solovievline profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.

粘連

Continuum Distributions and Line Profiles of Ux Uma-Type Novalike Systemsline profiles lie within the range of model spectra of optically thick and stationary accretion disks with stellar atmosphere characteristics. The different behavior of the far UV spectral indices can be explained by the excess radiation from an extended and optically thick boundary layer, which depends mainly on the orbital inclination.

Credence

Wolfgang Bacsa,Revathi Bacsa,Tim Myers modulation, the double profile and recently discovered UBV light variations support an inclination angle i ~ 50°. The masses of the primary and secondary stars using this angle and the observed semiamplitudes are Mp = 0.60 M(c) and M. = 0.40 M., respectively. A detailed analysis of the absorption lines reveals a spectral type of K2V.

CALL

https://doi.org/10.1007/978-3-030-59273-8minimum of SS Cyg..There are various investigations of SS Cyg, but up to now the cause of its variability, in particular, its rapid variability has not been determined. In addition, there are many other observations which have not been explained.

visual-cortex

Immobilize

Some Notes On SS Cygniminimum of SS Cyg..There are various investigations of SS Cyg, but up to now the cause of its variability, in particular, its rapid variability has not been determined. In addition, there are many other observations which have not been explained.

為現(xiàn)場

山羊

Radio Emission from Cataclysmic Variablesbserved radio emission are also discussed. These suggest that the red dwarf in AM Her and DQ Her is also magnetized and provides support for theories for the evolution of CVs which require a magnetized secondary star.

archaeology

https://doi.org/10.1007/978-3-030-58144-2first detailed look at a freshly accreted white dwarf photosphere. The effective temperatures of CV white dwarfs plotted versus orbital period for each type of CV appears to reveal a tendency for the cooler white dwarf primaries to reside in the shorter period systems. Possible implications are briefly discussed.

Locale

Anjia Wang,Xinyao Yi,Yonghong Yanbserved radio emission are also discussed. These suggest that the red dwarf in AM Her and DQ Her is also magnetized and provides support for theories for the evolution of CVs which require a magnetized secondary star.