VSX J074727.6+065050: a new WZ Sagittae star in Canis minor

Source: arXiv

ABSTRACT We present photometry of the first reported superoutburst of the dwarf nova VSX J074727.6+065050 during 2008 January and February. At its brightest the star reached magnitude 11.4 and this was followed by a slow decline at 0.09 mag/d for 19 days, corresponding to the plateau phase. There was then a rapid decline at 1.66 mag/d to a temporary minimum at magnitude 16.6 where it stayed for 2 to 3 days after which there were six remarkable echo outbursts before the star gradually faded back towards quiescence at ~magnitude 19.5. The overall outburst amplitude was at least 8 magnitudes and it lasted more than 80 days. During the plateau phase we observed common superhumps with Psh = 0.06070(6) d, but the period increased to Psh = 0.06151(5) d coinciding with the end of the plateau phase and the onset of the rapid decline. This corresponds to a continuous period change with P^dot = +4.4(9) x 10-5. During the echo outbursts there was a superhump regime with Psh = 0.06088(49) d. Evidence is presented which is consistent with the star being a member of the WZ Sge family of dwarf novae. Comment: 20 pages, 11 figures. Accepted for publication in the Journal of the British Astronomical Association

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Available from: Lewis Cook, Sep 27, 2015
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    ABSTRACT: High speed photometric observations of the dwarf nova VSX J074727.6 + 065050 made in December 2009 during quiescence show an orbital modulation at P orb =85.6 min. They also show that the star is a member of the relatively rare CV/ZZ group, i.e. the accreting white dwarf primary has non-radial pulsations. The two regions of oscillating power are at 684 s and 238 s. There is some evidence for hidden ∼1 µHz fine structure splitting, which has been seen in three other CV/ZZ stars.
    Astrophysics and Space Science 05/2011; 333(1):119-123. DOI:10.1007/s10509-010-0573-x · 2.26 Impact Factor