Identification of Nova Herculis 1960

On the Bright Line Spectrum of Nova Herculis.

HST / GHRS observations of AM Herculis ⋆

We present phase-resolved spectroscopy of AM Herculis obtained with the HST/GHRS when the system was in a high state. The ultraviolet light curve shows a quasi-sinusoidal modulation, which can be explained by a hot spot on the rotating white dwarf. The broad Lyα absorption expected for photospheric radiation of a moderately hot white dwarf is largely filled in with emission. The UV/FUV spectrum...

WZ Sagittae as a DQ Herculis star

We argue that quiescent WZ Sge is a rapidly spinning magnetic rotator in which most of the matter transfered from the secondary is ejected from the system. Assuming that the observed 27.87 s oscillation period is due to the spinning white dwarf we propose that the other observed principal period of 28.96 s is a beat due to reprocessing of the rotating white dwarf beam on plasma blobs in Kepleri...

Am Herculis Binaries in the Rosat Era

The current census of AM Herculis binaries and AM Her candidates exceeds 50 systems of which 29 are ROSAT discoveries. The increased number provides a basis to study the more general properties of the class. We discuss the space density, observations relevant to the evolution of magnetic CVs, the statistics of magnetic eld measurements, and current ideas on the accretion scenarios.

A Universal Decline Law of Classical Novae. Iv. V838 Her (1991): a Very Massive White Dwarf

We present a unified model of optical and ultraviolet (UV) light curves for one of the fastest classical novae, V838 Herculis (Nova Herculis 1991), and estimate its white dwarf (WD) mass. Based on an optically thick wind theory of nova outbursts, we model the optical light curves with free-free emission and the UV 1455 Å light curves with blackbody emission. Our models of 1.35 ± 0.02 M⊙ WD repr...