REFINED PROPERTIES OF THE HD 130322 PLANETARY SYSTEM
REFINED PROPERTIES OF THE HD 130322 PLANETARY SYSTEM
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HD 130322 行星系统的精致特性
DOI：
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
A. Howard
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文献类型：
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作者：
N. Hinkel;S. Kane;G. Henry;Y. K. Feng;T. Boyajian;J. Wright;D. Fischer;A. Howard
离太阳最近的系外行星系统拥有最明亮的宿主恒星，为宿主星星及其行星的特性研究提供了最有利的机会。中天星历精化和监测巡天使用新的径向速度测量和光度测量，以大大改善行星轨道的不确定性和星星的基本特性，在本例中是HD 130322。唯一的伴星HD 130322 b的轨道是相对圆形的，e = 0.029，每10.7天。我们已经编制了RV测量从多个来源，其中包括12个未发表的凯克我望远镜，在过去的2014年的过程中，并已减少了不确定性的过境中点到202小时。过境概率为b-同伴是4.7%，其中M p sin i = 1.15 M J？> a = 0.0925 Au。本文利用美国费尔伯恩天文台T11 0.8 m自动光电望远镜2004 - 2014年的测光资料，包括约束凌日窗，这导致了HD 130322 b在0.017等深度的完全凌日排除和在0.001等深度的掠凌日排除的决定性零结果。通过测光数据揭示了一个高度精确的恒星自转周期：26.53 ± 0.70天。此外，相对于比较恒星，宿主恒星的亮度与Ca ii H和K指数反相关，这是典型的年轻太阳型星星。
Exoplanetary systems closest to the Sun, with the brightest host stars, provide the most favorable opportunities for characterization studies of the host star and their planet(s). The Transit Ephemeris Refinement and Monitoring Survey uses both new radial velocity (RV) measurements and photometry in order to greatly improve planetary orbit uncertainties and the fundamental properties of the star, in this case HD 130322. The only companion, HD 130322b, orbits in a relatively circular orbit, e = 0.029 every ∼10.7 days. We have compiled RV measurements from multiple sources, including 12 unpublished from the Keck I telescope, over the course of ∼14 yr and have reduced the uncertainty in the transit midpoint to ∼2 hr. The transit probability for the b-companion is 4.7%, where M p sin i = 1.15 M J ?> and a = 0.0925 AU. In this paper, we compile photometric data from the T11 0.8 m Automated Photoelectric Telescope at Fairborn Observatory taken over ∼14 yr, including the constrained transit window, which results in a dispositive null result for both full transit exclusion of HD 130322b to a depth of 0.017 mag and grazing transit exclusion to a depth of ∼0.001 mag. Our analysis of the starspot activity via the photometric data reveals a highly accurate stellar rotation period: 26.53 ± 0.70 days. In addition, the brightness of the host with respect to the comparison stars is anti-correlated with the Ca ii H and K indices, typical for a young solar-type star.