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arXiv 0710.5701astro-ph
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新星V5116 Sgr和在新星遗迹中寻找超级驼峰

Nova V5116 Sgr and searching for superhumps in nova remnants

A. Dobrotka, A. Retter, A. Liu

备注：
9 pages, 7 figures, accepted for publication in A&A
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摘要：

我们提出的V5116 Sgr（新星Sgr 2005 #2）的未过滤的光度观测的周期分析，我们寻找超新星遗迹的超级驼峰候选人。周期分析采用PDM方法。新星成分的质量估计从第二质量-轨道周期和初级质量-下降时间的关系。我们发现2006年V5116 Sgr观测的13个夜晚都受到周期为$0.1238 \pm 0.0001$ d（$2.9712 \pm 0.0024$ h）的调制。根据相位光变曲线的形状，并且在数据的不同子样本中周期性的值没有明显的变化，我们将周期解释为轨道性质。双星系统则落在激变变星轨道周期分布的周期间隙内。从最大星等-下降率关系出发，利用观测到的下降率$t_{\rm 2} = 6.5 \pm 1.0$ d值，估算了$M_{\rm Vmax} = -8.85 \pm 0.04$等的最大绝对视星等。激变变星的质量-周期关系产生了大约为$0.26 \pm 0.05 {\rm M}_{\rm \odot}$的二次质量估计。我们认为V5116 Sgr是一个高倾角系统，显示出次级星的辐射效应。在潮汐半径范围内，不可能存在完全发育的吸积盘，其值低于$3.5 10^{10}$ cm。质量比估计在一些新星和存在或不存在的超级驼峰在这些系统中进行了比较，质量比极限为超级驼峰约0.35。我们发现，在大多数具有预期超级驼峰的新星中，尚未发现这种变化。因此，鼓励对这些系统进行更多的观察。

英文摘要：

We present the period analysis of unfiltered photometric observations of V5116 Sgr (Nova Sgr 2005 #2) and we search for superhump candidates in novae remnants. The PDM method for period analysis is used. The masses of the novae componets are estimated from the secondary mass -- orbital period and primary mass -- decline time relations. We found that 13 nights of V5116 Sgr observations in the year 2006 are modulated with a period of $0.1238 \pm 0.0001$ d ($2.9712 \pm 0.0024$ h). Following the shape of the phased light curves and no apparent change in the value of the periodicity in different subsamples of the data, we interpret the period as orbital in nature. The binary system then falls within the period gap of the orbital period distribution of cataclysmic variables. From the maximum magnitude -- rate of decline relation, we estimate the maximum absolute visual magnitude of $M_{\rm Vmax} = -8.85 \pm 0.04$ mag using the measured value of decline $t_{\rm 2} = 6.5 \pm 1.0$ d. The mass-period relation for cataclysmic variables yields a secondary mass estimate of about $0.26 \pm 0.05 {\rm M}_{\rm \odot}$. We propose that V5116 Sgr is a high inclination system showing an irradiation effect of the secondary star. No fully developed accretion disc up to the tidal radius with the value lower than $3.5 10^{10}$ cm is probable. The mass ratio was estimated in a few novae and the presence or absence of superhumps in these systems was compared with the mass ratio limit for superhumps of about 0.35. We found that in the majority of novae with expected superhumps, this variability has not been found yet. Therefore, more observations of these systems is encouraged.

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