Issue |
A&A
Volume 624, April 2019
|
|
---|---|---|
Article Number | A15 | |
Number of page(s) | 11 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201834275 | |
Published online | 02 April 2019 |
Kepler-411: a four-planet system with an active host star★
1
Yunnan Observatories, Chinese Academy of Sciences,
Kunming 650216,
PR China
e-mail: sunleilei@ynao.ac.cn, wangxb@ynao.ac.cn
2
Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences,
Kunming 650216,
PR China
3
University of Chinese Academy of Sciences,
Beijing 100049,
PR China
4
Hamburger Sternwarte, Universität Hamburg,
Gojenbergsweg 112,
21029 Hamburg, Germany
e-mail: pioannidis@hs.unihamburg.de
5
Department of Mathematical Sciences, Xian Jiaotong-Liverpool University (XJTLU), 111 Renai Road, Suzhou Dushu Lake Science and Education Innovation District,
Suzhou Industrial Park,
Suzhou 215123, PR China
Received:
19
September
2018
Accepted:
13
December
2018
We present a detailed characterization of the Kepler-411 system (KOI 1781). This system was previously known to host two transiting planets: one with a period of 3 days (R = 2.4 R⊕; Kepler-411b) and one with a period of 7.8 days (R = 4.4 R⊕; Kepler-411c), as well as a transiting planetary candidate with a 58-day period (R = 3.3 R⊕; KOI 1781.03) from Kepler photometry. Here, we combine Kepler photometry data and new transit timing variation (TTV) measurements from all the Kepler quarters with previous adaptive-optics imaging results, and dynamical simulations, in order to constrain the properties of the Kepler-411 system. From our analysis, we obtain masses of 25.6 ± 2.6 M⊕ for Kepler-411b and 26.4 ± 5.9 M⊕ for Kepler-411c, and we confirm the planetary nature of KOI 1781.03 with a mass of 15.2 ± 5.1 M⊕, hence the name Kepler-411d. Furthermore, by assuming near-coplanarity of the system (mutual inclination below 30°), we discover a nontransiting planet, Kepler-411e, with a mass of 10.8 ± 1.1 M⊕ on a 31.5-day orbit, which has a strong dynamical interaction with Kepler-411d. With densities of 1.71 ± 0.39 g cm−3 and 2.32 ± 0.83 g cm−3, both Kepler-411c and Kepler-411d belong to the group of planets with a massive core and a significant fraction of volatiles. Although Kepler-411b has a sub-Neptune size, it belongs to the group of rocky planets.
Key words: planets and satellites: dynamical evolution and stability / stars: activity / planetary systems / starspots
Tables 2–4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/624/A15
© ESO 2019
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