V729 Sgr: a long period dwarf nova showing negative superhumps during quiescence

被引:10
作者
Ramsay, Gavin [1 ]
Wood, Matt A. [2 ]
Cannizzo, John K. [3 ,4 ,5 ]
Howell, Steve B. [6 ]
Smale, Alan [7 ]
机构
[1] Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DG, North Ireland
[2] Texas A&M Univ Commerce, Dept Phys & Astron, Commerce, TX 75429 USA
[3] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA
[4] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA
[5] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA
[6] NASA, Ames Res Ctr, Moffett Field, CA 94095 USA
[7] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
基金
美国国家科学基金会;
关键词
accretion; accretion discs; stars: dwarf novae; stars: individual: V729 Sgr; novae; cataclysmic variables; X-RAY BINARIES; CATACLYSMIC VARIABLES; KEPLER OBSERVATIONS; SIMULATIONS; MISSION; SUPEROUTBURSTS; OUTBURSTS; EVOLUTION; STARS; FIELD;
D O I
10.1093/mnras/stx859
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report K2 observations of the eclipsing cataclysmic variable V729 Sgr which covered nearly 80 d in duration. We find five short outbursts and two long outbursts, one of which shows a clear plateau phase in the rise to maximum brightness. The mean time between successive short outbursts is similar to 10 d while the time between the two long outbursts is similar to 38 d. The frequency of these outbursts is unprecedented for a cataclysmic variable ( CV) above the orbital period gap. We find evidence that the mid-point of the eclipse occurs systematically earlier in outburst than in quiescence. During five of the six quiescent epochs we find evidence for a second photometric period which is roughly 5 per cent shorter than the 4.16 h orbital period which we attribute to negative superhumps. V729 Sgr is therefore one of the longest period CVs to show negative superhumps during quiescence.
引用
收藏
页码:950 / 955
页数:6
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