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EPIC 249624646: a warm Jupiter and a mini-Neptune in a triple-star system | | M. Hjorth
; A. B. Justesen
; T. Hirano
; S. Albrecht
; D. Gandolfi
; F. Dai
; R. Alonso
; O. Barragán
; M. Esposito
; M. Kuzuhara
; K. W. F. Lam
; J. H. Livingston
; P. Montanes-Rodriguez
; N. Narita
; G. Nowak
; J. Prieto-Arranz
; S. Redfield
; F. Rodler
; V. Van Eylen
; J. N. Winn
; G. Antoniciello
; J. Cabrera
; W. D. Cochran
; Sz. Csizmadia
; J. de Leon
; H. Deeg
; Ph. Eigmüller
; M. Endl
; A. Erikson
; M. Fridlund
; S. Grziwa
; E. Guenther
; A. P. Hatzes
; P. Heeren
; D. Hidalgo
; J. Korth
; R. Luque
; D. Nespral
; E. Palle
; M. Pätzold
; C. M. Persson
; H. Rauer
; A. M. S. Smith
; T. Trifonov
; | | Date: |
11 Jan 2019 | | Abstract: | We report the discovery of two transiting planets orbiting EPIC 249624646, a
bright (V=11.11) late F-type star residing in a triple-star system. It was
observed during Campaign 15 of the K2 mission, and in order to confirm and
characterise the system, follow-up spectroscopy and AO imaging were carried out
using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia
data we identify two M-dwarf companions at a separation of $113 pm 2$ AU and
$2467_{-155}^{+177}$ AU. From radial velocities, K2 photometry, and stellar
characterisation of the host star, we find the inner planet to be a
mini-Neptune with a radius of $3.06 pm 0.16 R_{oplus}$ and an orbital period
of $P = 9.2$ days. The radius of the mini-Neptune suggests that the planet is
located above the radius valley, and with an incident flux of $Fsim 400
F_{oplus}$, it lies safely outside the super-Earth desert. The outer warm
Jupiter has a mass of $0.774pm 0.047 M_{
m J}$ and a radius of $1.006pm
0.050R_{
m J}$, and orbits the host star every 48.4 days on an orbit with an
eccentricity $e<0.241$. Its mild eccentricity and mini-Neptune sibling suggest
that the warm Jupiter originates from in situ formation or disk migration. | | Source: | arXiv, 1901.3716 | | Services: | Forum | Review | PDF | Favorites | |
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