An independent planet search in the Kepler dataset - II. An extremely low-density super-Earth mass planet around Kepler-87
An independent planet search in the Kepler dataset - II. An extremely low-density super-Earth mass planet around Kepler-87
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开普勒数据集中的独立行星搜索 - II 开普勒 87 周围的极低密度超级地球质量行星
DOI：
10.1051/0004-6361/201220935
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发表时间：
2014
影响因子：
6.5
通讯作者：
Tim-Oliver
中科院分区：
文献类型：
--
作者：
Dreizler;Stefan;Zechmeister;Mathias;Husser;Tim-Oliver
开普勒计划的主要目标是测量类地行星围绕类日恒星运行的频率。然而，要在长时间内确认FGK矮星周围最小的开普勒候选行星是极其困难的，甚至超出了当前径向速度技术的极限。凌日时间变化（ttv）可能提供了通过行星之间的相互引力作用来证实近共振多系统的可能性。我们之前在KOI 1574系统中发现了第二颗候选行星。两个候选元素的周期相对较长（约114 d和191 d），共振为5:3。因此，我们在这个特别有前途的系统中寻找电视。方法利用已证实的SARS管道对全开普勒数据进行趋势分析。整个数据允许人们搜索上述信号的ttv，并搜索其他类似凌日的信号。结果我们检测到114 d和191 d信号的强反相关ttv，动态确认它们是同一系统的成员。动态模拟再现了观测到的ttv，这也使我们能够确定行星的质量。我们发现KOI 1574.01（以下简称Kepler-87 b）的半径为13.49±0.55R⊕，质量为324.2±8.8M⊕,KOI 1574.02 （Kepler-87 c）的半径为6.14±0.29R⊕，质量为6.4±0.8M⊕。这两颗行星的密度都很低，分别为0.729和0.152 g cm-3，这对于如此寒冷和古老（7 - 8 Gyr）的行星来说是非常重要的。具体来说，开普勒-87 c是超级地球质量范围内密度最低的行星。因此，这两颗行星都特别适合于建模和行星结构研究，并且也提出了一个有趣的案例，即开普勒行星的地面光度跟踪是非常可取的。最后，我们还在该系统中发现了另外两颗短周期超级地球大小（<2R⊕）的候选行星，这使得该系统的相对较高的多重性值得注意，而在开普勒-87 b等巨行星存在的情况下，多重系统的普遍缺乏。
ContextThe primary goal of theKeplermission is the measurement of the frequency of Earth-like planets around Sun-like stars. However, the confirmation of the smallest ofKepler’s candidates in long periods around FGK dwarfs is extremely difficult or even beyond the limit of current radial velocity technology. Transit timing variations (TTVs) may offer the possibility for these confirmations of near-resonant multiple systems by the mutual gravitational interaction of the planets.AimsWe previously detected the second planet candidate in the KOI 1574 system. The two candidates have relatively long periods (about 114 d and 191 d) and are in 5:3 resonance. We therefore searched for TTVs in this particularly promising system.MethodsThe fullKeplerdata was detrended with the proven SARS pipeline. The entire data allowed one to search for TTVs of the above signals, and to search for additional transit-like signals.ResultsWe detected strong anti-correlated TTVs of the 114 d and 191 d signals, dynamically confirming them as members of the same system. Dynamical simulations reproducing the observed TTVs allowed us to also determine the masses of the planets. We found KOI 1574.01 (hereafter Kepler-87 b) to have a radius of 13.49 ± 0.55R⊕and a mass of 324.2 ± 8.8M⊕, and KOI 1574.02 (Kepler-87 c) to have a radius of 6.14 ± 0.29R⊕and a mass of 6.4 ± 0.8M⊕. Both planets have low densities of 0.729 and 0.152 g cm-3, respectively, which is non-trivial for such cold and old (7−8 Gyr) planets. Specifically, Kepler-87 c is the lowest-density planet in the super-Earth mass range. Both planets are thus particularly amenable to modeling and planetary structure studies, and also present an interesting case where ground-based photometric follow-up ofKeplerplanets is very desirable. Finally, we also detected two more short-period super-Earth sized (<2R⊕) planetary candidates in the system, making the relatively high multiplicity of this system notable against the general paucity of multiple systems in the presence of giant planets like Kepler-87 b.
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影响因子：
7.9
作者：
Anglada-Escude, Guillem;Arriagada, Pamela;Jenkins, James S.
通讯作者：
Jenkins, James S.
DOI：
10.1111/j.1365-2966.2012.20467.x
发表时间：
2012-01
影响因子：
4.8
作者：
J. Steffen;D. Fabrycky;E. Ford;J. Carter;J. Désert;F. Fressin;M. Holman;J. Lissauer;A. Moorhead;J. Rowe;D. Ragozzine;W. Welsh;N. Batalha;W. Borucki;L. Buchhave;S. Bryson;D. Caldwell;D. Charbonneau;D. Ciardi;W. Cochran;M. Endl;M. Everett;T. Gautier;R. Gilliland;F. Girouard;J. Jenkins;E. Horch;S. Howell;H. Isaacson;T. Klaus;D. Koch;D. Latham;Jie Li;P. Lucas;P. Macqueen;G. Marcy;S. McCauliff;C. Middour;R. Morris;F. Mullally;S. Quinn;E. Quintana;Avi Shporer;M. Still;P. Tenenbaum;S. Thompson;J. Twicken;Jeffery Van Cleve Fermilab Center for Particle Astrophysics-Jeffery-Van-Cleve-Fermilab-Center-for-Particle-2302795556;Batavia;IL UCOLick Observatory;U. California;Santa Cruz Hubble Fellow Astronomy Department;U. Florida;H. C. F. Astrophysics;N. R. Center;Seti Institute Nasa Exoplanet Science InstituteCaliforn Technology-Seti-Institute-Nasa-Exoplanet-Science-Technology-102260141;A. Department;San Diego State University;San Diego State University;J. V. R. I. O. Technology;C. F. Research;U. Hertfordshire;Berkeley;B. A. E. R. I. A. R. Center-B.-A.-E.-R.-I.-A.-R.-Center-103192896;National Optical Astronomy Observatory;D. Physics;Southern Connecticut State University;Las Cumbres Observatory Global Telescope;Niels Bohr Institute;Copenhagen University;M. Observatory;The University of Texas;Space Telescope Science Institute;Baltimore.;O. Center
通讯作者：
J. Steffen;D. Fabrycky;E. Ford;J. Carter;J. Désert;F. Fressin;M. Holman;J. Lissauer;A. Moorhead;J. Rowe;D. Ragozzine;W. Welsh;N. Batalha;W. Borucki;L. Buchhave;S. Bryson;D. Caldwell;D. Charbonneau;D. Ciardi;W. Cochran;M. Endl;M. Everett;T. Gautier;R. Gilliland;F. Girouard;J. Jenkins;E. Horch;S. Howell;H. Isaacson;T. Klaus;D. Koch;D. Latham;Jie Li;P. Lucas;P. Macqueen;G. Marcy;S. McCauliff;C. Middour;R. Morris;F. Mullally;S. Quinn;E. Quintana;Avi Shporer;M. Still;P. Tenenbaum;S. Thompson;J. Twicken;Jeffery Van Cleve Fermilab Center for Particle Astrophysics-Jeffery-Van-Cleve-Fermilab-Center-for-Particle-2302795556;Batavia;IL UCOLick Observatory;U. California;Santa Cruz Hubble Fellow Astronomy Department;U. Florida;H. C. F. Astrophysics;N. R. Center;Seti Institute Nasa Exoplanet Science InstituteCaliforn Technology-Seti-Institute-Nasa-Exoplanet-Science-Technology-102260141;A. Department;San Diego State University;San Diego State University;J. V. R. I. O. Technology;C. F. Research;U. Hertfordshire;Berkeley;B. A. E. R. I. A. R. Center-B.-A.-E.-R.-I.-A.-R.-Center-103192896;National Optical Astronomy Observatory;D. Physics;Southern Connecticut State University;Las Cumbres Observatory Global Telescope;Niels Bohr Institute;Copenhagen University;M. Observatory;The University of Texas;Space Telescope Science Institute;Baltimore.;O. Center
DOI：
10.1088/0004-637x/750/2/113
发表时间：
2012-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
E. Ford;D. Fabrycky;J. Steffen;J. Carter;F. Fressin;M. Holman;J. Lissauer;A. Moorhead;R. C. Morehead;D. Ragozzine;J. Rowe;W. Welsh;C. Allen;N. Batalha;W. Borucki;S. Bryson;L. Buchhave;C. Burke;D. Caldwell;D. Charbonneau;B. Clarke;W. Cochran;J. D'esert;M. Endl;M. Everett;D. Fischer;T. Gautier;R. Gilliland;J. Jenkins;M. Haas;E. Horch;S. Howell;K. Ibrahim;H. Isaacson;D. Koch;D. Latham;Jie Li;P. Lucas;P. Macqueen;G. Marcy;S. McCauliff;F. Mullally;S. Quinn;E. Quintana;Avi Shporer;M. Still;P. Tenenbaum;S. Thompson;G. Torres;J. Twicken;Bill Wohler University of Florida;UCOLick Observatory;Hubble Fellow;F. C. F. P. Astrophysics-F.-C.-F.-P.-Astrophysics-103075200;H. C. F. Astrophysics;N. Ames;S. Institute;San Diego State University;O. Center;San Diego State University;Niels Bohr Institute;Natural History Museum of Denmark;M. Observatory;Noao;Yale University;JPLCaltech;Stsci;Southern Connecticut State University;U. California;Berkeley;U. Hertfordshire;Las Cumbres Observatory Global Telescope;Santa Barbara;B. A. E. R. I. A. R. Center-B.-A.-E.-R.-I.-A.-R.-Center-103192896
通讯作者：
E. Ford;D. Fabrycky;J. Steffen;J. Carter;F. Fressin;M. Holman;J. Lissauer;A. Moorhead;R. C. Morehead;D. Ragozzine;J. Rowe;W. Welsh;C. Allen;N. Batalha;W. Borucki;S. Bryson;L. Buchhave;C. Burke;D. Caldwell;D. Charbonneau;B. Clarke;W. Cochran;J. D'esert;M. Endl;M. Everett;D. Fischer;T. Gautier;R. Gilliland;J. Jenkins;M. Haas;E. Horch;S. Howell;K. Ibrahim;H. Isaacson;D. Koch;D. Latham;Jie Li;P. Lucas;P. Macqueen;G. Marcy;S. McCauliff;F. Mullally;S. Quinn;E. Quintana;Avi Shporer;M. Still;P. Tenenbaum;S. Thompson;G. Torres;J. Twicken;Bill Wohler University of Florida;UCOLick Observatory;Hubble Fellow;F. C. F. P. Astrophysics-F.-C.-F.-P.-Astrophysics-103075200;H. C. F. Astrophysics;N. Ames;S. Institute;San Diego State University;O. Center;San Diego State University;Niels Bohr Institute;Natural History Museum of Denmark;M. Observatory;Noao;Yale University;JPLCaltech;Stsci;Southern Connecticut State University;U. California;Berkeley;U. Hertfordshire;Las Cumbres Observatory Global Telescope;Santa Barbara;B. A. E. R. I. A. R. Center-B.-A.-E.-R.-I.-A.-R.-Center-103192896
优化长时间序列中凌日行星的搜索
影响因子：
6.5
作者：
通讯作者：
--
影响因子：
8.7
作者：
Batalha, Natalie M.;Rowe, Jason F.;Welsh, William F.
通讯作者：
Welsh, William F.