WARM JUPITERS ARE LESS LONELY THAN HOT JUPITERS: CLOSE NEIGHBORS

WARM JUPITERS ARE LESS LONELY THAN HOT JUPITERS: CLOSE NEIGHBORS
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DOI:
10.3847/0004-637x/825/2/98
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发表时间:
2016-01
期刊:
The Astrophysical Journal
影响因子:
--
通讯作者:
Chelsea X. Huang;Yanqin Wu;A. Triaud
Chelsea X. Huang;Yanqin Wu;A. Triaud
中科院分区:
其他
文献类型:
--
作者:
Chelsea X. Huang;Yanqin Wu;A. Triaud

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利用开普勒凌日数据,我们发现了亚木星伴星在包含热木星(HJS)(周期向内10天)和那些拥有暖木星(WJS)(周期在10天到200天之间)的系统之间的显著差异。HJS,除了WASP-47B,没有任何可探测到的内行星或外行星伴星(周期向内50天,大小到2地球)。把我们自己限制在内心的伙伴里,我们的极限可以达到1地球。与此形成鲜明对比的是,《华尔街日报》中有一半的人身边都是小伙伴。从统计上看,HOT和WJS的伴随分数是相互排斥的,特别是关于内部同伴。WJS的高伴生组分也为它们的形成提供了线索。有近亲的WJS应该具有低的轨道偏心率和低的相互倾角。这些系统的轨道构型让人想起开普勒任务大量发现的低质量近距离行星系统。这一点,以及其他论点,使我们提出这些WJS是在原地形成的。有迹象表明,可能存在具有不同特征的第二群WJS。在这张图中,WASP-47B可以被认为是原位WJS进入HJ区的延伸尾部,并不代表HJS的一般形成路线。
Exploiting the Kepler transit data, we uncover a dramatic distinction in the prevalence of sub-Jovian companions between systems that contain hot Jupiters (HJs) (periods inward of 10 days) and those that host warm Jupiters (WJs) (periods between 10 and 200 days). HJs, with the singular exception of WASP-47b, do not have any detectable inner or outer planetary companions (with periods inward of 50 days and sizes down to 2 REarth). Restricting ourselves to inner companions, our limits reach down to 1 REarth. In stark contrast, half of the WJs are closely flanked by small companions. Statistically, the companion fractions for hot and WJs are mutually exclusive, particularly in regard to inner companions. The high companion fraction of WJs also yields clues to their formation. The WJs that have close-by siblings should have low orbital eccentricities and low mutual inclinations. The orbital configurations of these systems are reminiscent of those of the low-mass close-in planetary systems abundantly discovered by the Kepler mission. This, and other arguments, lead us to propose that these WJs are formed in situ. There are indications that there may be a second population of WJs with different characteristics. In this picture, WASP-47b could be regarded as the extending tail of the in situ WJs into the HJ region and does not represent the generic formation route for HJs.