1,127 research outputs found
The new AM CVn star in Hydra
High speed photometry of the new AM CVn star in Hya (previously known as
SN2003aw), spectroscopically identified by Chornock & Filippenko, shows it to
have a superhump period of 2041.5 +/- 0.3 s. We find a range of brightness from
V ~ 16.5 to 20.3, presumably caused by variations in the rate of mass transfer.
In the intermediate state the system cycles in brightness with a period of ~ 16
h and range >= 0.4 mag. There are sidebands to the principal frequencies in the
Fourier transform which have constant frequency difference from the superhump
harmonics.Comment: 5 pages, 6 figures. Accepted for publication in MNRA
Rapid Oscillations in Cataclysmic Variables, and a Comparison with X-Ray Binaries
We compare some of the properties of rapid oscillations in cataclysmic
variables and X-Ray binaries. In addition to the earlier recognition that both
types possess the same correlation between high and low frequency
quasi-periodic oscillations, we have now found that the dwarf nova VW Hyi in
its late stages of outburst shows the 1:2:3 oscillations harmonics that are
seen in some neutron star and black hole X-Ray binaries. We point out that the
behaviour of the dwarf nova WZ Sge has some similarities to those of accreting
millisecond pulsars.Comment: 10 pages, 4 figures (needs AIP style file). To appear in the
conference proceedings of `Interacting Binaries: Accretion, Evolution &
Outcomes' (Cefalu, July 4-10 2004
General Properties of Quiescent Novae
The observed properties of novae before and after eruption are discussed. The
distribution of orbital periods of novae shows a concentration near 3.2 h,
which resembles that of magnetic cataclysmic variables, and there is some
evidence that many of the novae themselves are magnetic near that orbital
period. Desynchronisation of polars by nova eruptions can lead to an estimate
(~2 x 10^3 y) for the time between eruptions for the strongly magnetic systems;
this is much shorter than that found from other methods. The similarity of pre-
and post-nova luminosities, at high rates of mass transfer, is ascribed to
irradiation of the secondary producing a self-sustained high Mdot state. This
slows cooling of the white dwarf after eruption, delays the onset of full scale
dwarf nova outbursts in most systems, and delays any descent into a hibernation
state of low rate of mass transfer.Comment: 13 pages, 1 figure; To appear in the proceedings of `Classical Nova
Explosions', Sitges, Spai
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