UBVRI photopolarimetry of the long period eclipsing AM Herculis binary V1309

Details UBVRI photopolarimetry of the long period eclipsing AM Herculis binary V1309 UBVRI photopolarimetry of the long period eclipsing AM Herculis binary V1309

2002-12-03

arxiv.org/abs/astro-ph/0212066v1

Mon.Not.Roy.Astron.Soc. 340 (2003) 1

Astronomy and Astrophysics

Astrophysics

11 pages, 12 figures (2 colour), Fig1 and Fig 4 are in lower resolution than in original paper, accepted for publication in Mo

Scientific paper

10.1046/j.1365-8711.2003.06280.x

We report simultaneous UBVRI photo-polarimetric observations of the long period (7.98 h) AM Her binary V1309 Ori. The length and shape of the eclipse ingress and egress varies from night to night. We suggest this is due to the variation in the brightness of the accretion stream. By comparing the phases of circular polarization zero-crossovers with previous observations, we confirm that V1309 Ori is well synchronized, and find an upper limit of 0.002 percent for the difference between the spin and orbital periods. We model the polarimetry data using a model consisting of two cyclotron emission regions at almost diametrically opposite locations, and centered at colatitude 35 (deg) and 145 (deg) on the surface of the white dwarf. We also present archive X-ray observations which show that the negatively polarised accretion region is X-ray bright.

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