青年系外行星过境倡议（YETI）
Young Exoplanet Transit Initiative (YETI)
摘要：
我们提出了年轻系外行星过境倡议（YETI），其中我们使用世界各地的几个0.2至2.6米望远镜连续监测年轻（<1亿年），附近（< 1千秒差距）的星团主要是为了检测年轻的过境行星（并研究其他变化现象的时间尺度从分钟到年）。望远镜网络使我们能够连续几天观察目标，以免错过任何凌日。运行通常为一到两周长，在随后的两三年内，每个集群每年运行大约三次，大约十个集群。在每个区域都有数千颗可探测到的恒星，其中有数百个已知的星团成员，例如，在观测到的第一个星团Tr-37中，YETI调查的典型星团，在YETI数据中至少有469颗已知的年轻恒星，其亮度低至R=16.5等，精度足以达到50毫等rms（5 mmag rms下降到R=14.5 mag）来检测凌日，因此我们可以预期在这个星团中至少有一个年轻的凌日天体。如果我们观察10个类似的星团，我们可以预期检测到大约10个具有半径测定的年轻凌日行星。上面给出的精度是针对YETI网络的一个典型望远镜，即60/90厘米耶拿望远镜（其他望远镜的亮度极限相似，即在+/-1等以内），以便可以探测到行星凌日。对于质量和半径确定的行星，我们可以计算平均密度并探测内部结构。我们的目标是通过发现年龄小于1亿年的行星来限制行星形成模型及其时间尺度，不仅要确定它们的轨道参数，还要测量它们的真实质量和半径，这到目前为止只有通过凌日法才有可能。在这里，我们提出了一个概述和第一个结果。（摘要缩短）
英文摘要：
We present the Young Exoplanet Transit Initiative (YETI), in which we use several 0.2 to 2.6m telescopes around the world to monitor continuously young (< 100 Myr), nearby (< 1 kpc) stellar clusters mainly to detect young transiting planets (and to study other variability phenomena on time-scales from minutes to years). The telescope network enables us to observe the targets continuously for several days in order not to miss any transit. The runs are typically one to two weeks long, about three runs per year per cluster in two or three subsequent years for about ten clusters. There are thousands of stars detectable in each field with several hundred known cluster members, e.g. in the first cluster observed, Tr-37, a typical cluster for the YETI survey, there are at least 469 known young stars detected in YETI data down to R=16.5 mag with sufficient precision of 50 milli-mag rms (5 mmag rms down to R=14.5 mag) to detect transits, so that we can expect at least about one young transiting object in this cluster. If we observe 10 similar clusters, we can expect to detect approximately 10 young transiting planets with radius determinations. The precision given above is for a typical telescope of the YETI network, namely the 60/90-cm Jena telescope (similar brightness limit, namely within +/-1 mag, for the others) so that planetary transits can be detected. For planets with mass and radius determinations, we can calculate the mean density and probe the internal structure. We aim to constrain planet formation models and their time-scales by discovering planets younger than 100 Myr and determining not only their orbital parameters, but also measuring their true masses and radii, which is possible so far only by the transit method. Here, we present an overview and first results. (Abstract shortened)
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