Characterization of the planetary system Kepler-101 with HARPS-N: a hot super-Neptune with an Earth-sized low-mass companion
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We characterize the planetary system Kepler-101 by performing a combined
differential evolution Markov chain Monte Carlo analysis of Kepler data
and forty radial velocities obtained with the HARPS-N spectrograph.
This system was previously validated and is composed of a hot
super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c.
These two planets orbit the slightly evolved and metal-rich G-type star
in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3,
Kepler-101b is the first fully characterized super-Neptune, and its
density suggests that heavy elements make up a significant fraction of
its interior; more than 60% of its total mass. Kepler-101c has a radius
of 1.25-0.17+ 0.19 R⊕,
which implies the absence of any H/He envelope, but its mass could not
be determined because of the relative faintness of the parent star for
highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp< 3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 − containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance −
is certainly of interest for scenarios of planet formation and
evolution. This system does not follow thepreviously reported trend that
the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet.
Translated title of the contribution | A hot super-Neptune with an Earth-sized low-mass companion |
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Original language | English |
Article number | A2 |
Journal | Astronomy & Astrophysics |
Volume | 572 |
Number of pages | 7 |
ISSN | 0004-6361 |
DOIs | |
Publication status | Published - 2014 |
ID: 138811613