The photometric period in ES Ceti The photometric period in ES Ceti
The photometric period in ES Ceti The photometric period in ES Ceti
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ES Ceti 中的光度周期 ES Ceti 中的光度周期
DOI：
10.1111/j.1365-2966.2011.18382.x
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发表时间：
2011
影响因子：
4.8
通讯作者：
Copperwheat C
中科院分区：
文献类型：
--
作者：
Copperwheat C
我们提出了ULTRACAM测光的ESCet，一个超紧凑的二进制620秒的轨道周期。像这样的系统中的质量转移被认为是由引力辐射驱动的，这导致双星演化到更长的周期，因为半生成的供体星星在失去质量时会膨胀。我们补充这些ULTRACAM+威廉赫歇尔望远镜（WHT）的数据与世界各地的小型望远镜在9年的基线观测。所有的观测都显示了轨道周期的变化，通过对这种变化进行计时，我们跟踪了这个系统的周期演化。我们没有检测到任何显着偏离线性星历，这意味着一个捐助者星星，是小质量和接近完全简并状态。这一发现支持了这颗犬座AM（AM CVn）星星的双白色矮星形成通道。另一种解释是，该系统处于相对短暂的阶段，其中传质速率向其长期值攀升。
We present ULTRACAM photometry of ES Cet, an ultracompact binary with a 620-s orbital period. The mass transfer in systems such as this one is thought to be driven by gravitational radiation, which causes the binary to evolve to longer periods since the semidegenerate donor star expands in size as it loses mass. We supplement these ULTRACAM+William Herschel Telescope (WHT) data with observations made with smaller telescopes around the world over a 9-yr baseline. All of the observations show variation on the orbital period, and by timing this variation we track the period evolution of this system. We do not detect any significant departure from a linear ephemeris, implying a donor star that is of small mass and close to a fully degenerate state. This finding favours the double white dwarf formation channel for this AM Canum Venaticorum (AM CVn) star. An alternative explanation is that the system is in the relatively short-lived phase in which the mass transfer rate climbs towards its long-term value.