Abstract
The population of cataclysmic variables with orbital periods right above the period gap are dominated by systems with extremely high mass transfer rates, the so-called SW Sextantis stars. On the other hand, some old novae in this period range which are expected to show high mass transfer rate instead show photometric and/or spectroscopic resemblance to low mass transfer systems like dwarf novae. We discuss them as candidates for so-called hibernating systems, CVs that changed their mass transfer behaviour due to a previously experienced nova outburst. This paper is designed to provide input for further research and discussion as the results as such are still very preliminary.
Highlights
In the following we briefly review our current knowledge on the populations of old novae and SW Sextantis stars especially in the context of the evolution of cataclysmic variable stars (CVs)
The mass transfer is greatly diminished which allows the secondary star to relax into a state of thermal equilibrium and to contract to a volume corresponding to its mass
Some potential evidence for hibernation has been presented in the form of old nova shells around CVs that have previously been known as low mass transfer systems, i.e. Z Cam (Shara et al, 2007) and AT Cnc (Shara et al, 2012)
Summary
In the following we briefly review our current knowledge on the populations of old novae and SW Sextantis stars especially in the context of the evolution of cataclysmic variable stars (CVs). For an extensive review of the current understanding of CV evolution, see Knigge et al ̃(2011)
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