One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c
One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c
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DOI：
10.1051/0004-6361/201526008
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发表时间：
2015-03
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通讯作者：
David J Armstrong;A. Santerne;D. Veras;S. Barros;O. Demangeon;J. Lillo-Box;J. McCormac;H. Osborn;M. Tsantaki;J. Almenara;D. Barrado;I. Boisse;A. Bonomo;F. Bouchy;David J. A. Brown;G. Bruno;J. R. Cerda;B. Courcol;M. Deleuil;R. D'iaz;A. Doyle;G. H'ebrard;J. Kirk;K. Lam;D. Pollacco;A. Rajpurohit;J. Spake;S. Walker
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作者：
David J Armstrong;A. Santerne;D. Veras;S. Barros;O. Demangeon;J. Lillo-Box;J. McCormac;H. Osborn;M. Tsantaki;J. Almenara;D. Barrado;I. Boisse;A. Bonomo;F. Bouchy;David J. A. Brown;G. Bruno;J. R. Cerda;B. Courcol;M. Deleuil;R. D'iaz;A. Doyle;G. H'ebrard;J. Kirk;K. Lam;D. Pollacco;A. Rajpurohit;J. Spake;S. Walker
目标。 K2 任务最近开始发现新的、多样化的行星系统。 2014 年 12 月，发布了该任务的“活动 1”数据，在 80 天的时间内为大约 22,000 个物体提供了高精度光度测量。我们搜索这些数据的目的是检测更重要的新物体。方法。我们通过两个独立的管道进行搜索，独立发现了 K2-19b 和 c，这是一个由海王星大小的天体（4.2 和 7.2 R 圆加号）组成的两行星系统，围绕 K 矮星运行，其平均运动共振非常接近 3:2。这两颗行星各自表现出凌日，有时由于它们接近共振和合相而同时出现。结果。我们使用 NITES 望远镜对较大行星进行了进一步的地面光度测量，证明了大的凌日时间变化 (TTV) 的存在，并使用观测到的 TTV 对凌日天体施加质量约束，假设这些天体位于附近但未共振。然后我们通过 PASTIS 工具对行星进行了统计验证，
Aims. The K2 mission has recently begun to discover new and diverse planetary systems. In December 2014, Campaign 1 data from the mission was released, providing high-precision photometry for similar to 22 000 objects over an 80-day timespan. We searched these data with the aim of detecting more important new objects. Methods. Our search through two separate pipelines led to the independent discovery of K2-19b and c, a two-planet system of Neptune-sized objects (4.2 and 7.2 R-circle plus), orbiting a K dwarf extremely close to the 3: 2 mean motion resonance. The two planets each show transits, sometimes simultaneously owing to their proximity to resonance and the alignment of conjunctions. Results. We obtained further ground-based photometry of the larger planet with the NITES telescope, demonstrating the presence of large transit timing variations (TTVs), and used the observed TTVs to place mass constraints on the transiting objects under the hypothesis that the objects are near but not in resonance. We then statistically validated the planets through the PASTIS tool,