High speed photometry of faint Cataclysmic Variables: III. V842 Cen, BY Cir, DD Cir, TV Crv, V655 CrA, CP Cru, V794 Oph, V992 Sco, EU Sct and V373 Sct

Details High speed photometry of faint Cataclysmic Variables: III. V842 Cen, BY Cir, DD Cir, TV Crv, V655 CrA, CP Cru, V794 Oph, V992 Sco, EU Sct and V373 Sct High speed photometry of faint Cataclysmic Variables: III. V842 Cen, BY Cir, DD Cir, TV Crv, V655 CrA, CP Cru, V794 Oph, V992 Sco, EU Sct and V373 Sct

2003-01-14

arxiv.org/abs/astro-ph/0301241v1

Mon.Not.Roy.Astron.Soc. 340 (2003) 1011

Astronomy and Astrophysics

Astrophysics

10 pages, 16 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06367.x

We present further results from a high speed photometric survey of faint cataclysmic variables. We find that V842 Cen (Nova Cen 1986 No. 2) is highly active, but with no evident orbital modulation. BY Cir (Nova Cir 1995) is an eclipsing system with an orbital period P(orb) of 6.76 h. TV Crv, an SU UMa type dwarf nova, is found to have P(orb) = 1.509 h from photometry at quiescence. DD Cir (Nova Cir 1999) is an eclipsing system with P(orb) = 2.339 h, a possible secondary eclipse, and a ~670 s photometric modulation. V655 CrA is highly active but shows no orbital modulation. The identification of V794 Oph is probably incorrect as we find no photometric variability. CP Cru (Nova Cru 1996) is an eclipsing system with P(orb) = 22.7 h. V992 Sco has P(orb) = 3.686 h from its periodic modulation. The supposed identification of EU Sct is probably incorrect. And finally, during one run V373 Sct (Nova Sct 1975) had a 258.3 s coherent periodicity, making it a candidate DQ Herculis star.

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