VV Pup the polar
Observed: 25, 31 Jan, 1 Feb 2006
8 Feb 2006
Updated 29 Dec 2007 (phase origin)
Light curves for this cataclysmic polar are presented.
VV Pup is a cataclysmic system, that is a binary with an accreting white
dwarf. The white dwarf is strongly magnetized (about 10^8 gauss), its
spin is synchronized with the orbital motion, and the accretion is funneled
by the magnetic field (no accretion disk). This type of cataclysmic is
a polar or an AM Her. The orbital/spin period is 100.44 mn, the distance
145 pc (Warner (1995)).
The observations were carried out with a 203 mm f/6.3 SC telescope,
a filter wheel and a SBIG ST7E camera. Each exposure is 200s long.
A Clear filter was used for the 25 Jan session.
For the 31 Jan and 1 Feb sessions, two perpendicular polarized filters
were used alternatively. This was in a vain attempt at observing
VV Pup polarization (Warner (1995) page 333).
The comparison star is GSC 6004-03141 with an assumed magnitude of 13.000
whatever the filter. The check star is an anonymous star at RA=08:15:12.93,
DEC=-19:02:14.3, with an observed average unfiltered magnitude of 15.104
(standard deviation 0.047), with one of the polarization filter 15.124
(0.058) and with the other polarization filter 15.101 (0.068).
The light curves:
UNFILTERED. Red: VV Pup. Blue: the check star, shifted by +1.5 mag.
The error bars are +/- the 1-sigma statistical uncertainties.
POLARIZED. Red: polarizer parallel to the DEC axis, Blue: parallel to the RA axis.
POLARIZED. Red: polarizer at 45° from the RA/DEC axes, Blue: perpendicular
to the first filter.
The data may be folded with the orbital/spin period:
Green: unfiltered. Blue, red: polarization filters.
The phase is computed for a period of 0.069747d and 2,453,000.0 as the origin.
Warner B. (1995) Cataclysmic Variable Stars Cambridge UP.
Telescope and camera configuration.
Computer and software configuration.
2007 follow up observations.