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arXiv 1206.6709astro-ph.SR
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DWARF项目：观测双星--发现系外行星的精确时钟

The DWARF project: Eclipsing binaries - precise clocks to discover exoplanets

T. Pribulla, M. Vaňko, M. Ammler - von Eiff, M. Andreev, A. Aslantürk, N. Awadalla, D. Baluďanský, A. Bonanno, H. Božić, G. Catanzaro, L. Çelik, P. E. Christopo… 展开作者

T. Pribulla, M. Vaňko, M. Ammler - von Eiff, M. Andreev, A. Aslantürk, N. Awadalla, D. Baluďanský, A. Bonanno, H. Božić, G. Catanzaro, L. Çelik, P. E. Christopoulou, E. Covino, F. Cusano, D. Dimitrov, P. Dubovský, E. M. Esmer, A. Frasca, Ľ. Hambálek, M. Hanna, A. Hanslmeier, B. Kalomeni, D. P. Kjurkchieva, V. Krushevska, I. Kudzej, E. Kundra, Yu. Kuznyetsova, J. W. Lee, M. Leitzinger, G. Maciejewski, D. Moldovan, M. H. M. Morais, M. Mugrauer, R. Neuhäuser, A. Niedzielski, P. Odert, J. Ohlert, İ. Özavcı, A. Papageorgiou, Š. Parimucha, S. Poddaný, A. Pop, M. Raetz, S. Raetz, Ya. Romanyuk, D. Ruždjak, J. Schulz, H. V. Şenavcı, T. Szalai, P. Székely, D. Sudar, C. T. Tezcan, M. E. Törün, V. Turcu, O. Vince, M. Zejda

备注：
12 pages, 2 figures, submitted to Astron. Nachrichten
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摘要：

我们提出了一个新的观测活动，DWARF，旨在使用低质量食双星的最小值的时间来检测太阳系外行星。观测将在一个由孔径约为20-200厘米的相对中小型望远镜组成的广泛网络内进行。要监测的天体的初始样本包含（i）具有M和K分量的低质量食双星，（ii）具有sdB或sdO分量的短周期双星，以及（iii）包含WD的后公共包络系统，这使得能够以高精度确定最小值。由于定时信号的幅度随着不可见第三分量的轨道周期而增加，因此项目的时间尺度很长，至少需要5-10年。本文给出了估算食双星对环联星探测适宜性的简单公式。双星的内禀变率（光球斑、耀斑、脉动等）还讨论了限制最小定时的精度。该手稿还描述了最佳观测策略和方法，以检测周期性的时间变化，在最小的时间表明存在的环联行星。对选定的目标进行了首次试验观测。

英文摘要：

We present a new observational campaign, DWARF, aimed at detection of circumbinary extrasolar planets using the timing of the minima of low-mass eclipsing binaries. The observations will be performed within an extensive network of relatively small to medium-size telescopes with apertures of ~20-200 cm. The starting sample of the objects to be monitored contains (i) low-mass eclipsing binaries with M and K components, (ii) short-period binaries with sdB or sdO component, and (iii) post-common-envelope systems containing a WD, which enable to determine minima with high precision. Since the amplitude of the timing signal increases with the orbital period of an invisible third component, the timescale of project is long, at least 5-10 years. The paper gives simple formulas to estimate suitability of individual eclipsing binaries for the circumbinary planet detection. Intrinsic variability of the binaries (photospheric spots, flares, pulsation etc.) limiting the accuracy of the minima timing is also discussed. The manuscript also describes the best observing strategy and methods to detect cyclic timing variability in the minima times indicating presence of circumbinary planets. First test observation of the selected targets are presented.

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