2014A&A...572A...2B


Query : 2014A&A...572A...2B

2014A&A...572A...2B - Astronomy and Astrophysics, volume 572A, 2-2 (2014/12-1)

Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion.

BONOMO A.S., SOZZETTI A., LOVIS C., MALAVOLTA L., RICE K., BUCHHAVE L.A., SASSELOV D., CAMERON A.C., LATHAM D.W., MOLINARI E., PEPE F., UDRY S., AFFER L., CHARBONNEAU D., COSENTINO R., DRESSING C.D., DUMUSQUE X., FIGUEIRA P., FIORENZANO A.F.M., GETTEL S., HARUTYUNYAN A., HAYWOOD R.D., HORNE K., LOPEZ-MORALES M., MAYOR M., MICELA G., MOTALEBI F., NASCIMBENI V., PHILLIPS D.F., PIOTTO G., POLLACCO D., QUELOZ D., SEGRANSAN D., SZENTGYORGYI A. and WATSON C.

Abstract (from CDS):

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 +5.1M, radius Rp=5.77–0.79+0.85R, and density ρp=1.45–0.48+0.83g/cm3, 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+0.19R, 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<3.8M, 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 the previously 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.

Abstract Copyright:

Journal keyword(s): planetary systems - stars: fundamental parameters - techniques: photometric - techniques: radial velocities - techniques: spectroscopic

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HAT-P-26b Pl 14 12 37.5331103311 +04 03 36.116569918           ~ 153 1
2 HAT-P-18b Pl 17 05 23.1475847690 +33 00 44.939145027           ~ 105 1
3 Kepler-101 Er* 18 53 01.3205511624 +48 21 18.784380528   14.474 13.729 13.574   ~ 47 0
4 Kepler-101b Pl 18 53 01.3205769348 +48 21 18.783753709           ~ 46 0
5 Kepler-101c Pl 18 53 01.3205769348 +48 21 18.783753709           ~ 22 0
6 Kepler-9b Pl 19 02 17.7544105084 +38 24 03.177247136           ~ 103 1
7 Kepler-25b Pl 19 06 33.2143323702 +39 29 16.357969502           ~ 63 1
8 CoRoT-8b Pl 19 26 21.2426686221 +01 25 35.178176730           ~ 51 1
9 Kepler-56b Pl 19 35 02.0013983772 +41 52 18.691751459           ~ 57 1
10 Kepler-35b Pl 19 37 59.2726236478 +46 41 22.952068619           ~ 87 1
11 Kepler-89d Pl 19 49 19.9344504805 +41 53 28.005888625           ~ 81 1
12 Kepler-89e Pl 19 49 19.9344504805 +41 53 28.005888625           ~ 61 1
13 Kepler-87c Pl 19 51 40.0490992347 +46 57 54.427022288           ~ 45 1
14 Kepler-18c Pl 19 52 19.0688249829 +44 44 46.807526602           ~ 74 1

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2023.09.26-02:29:51

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