2020A&A...641A..68B


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.05CET00:57:31

2020A&A...641A..68B - Astronomy and Astrophysics, volume 641A, 68-68 (2020/9-1)

The GAPS programme at TNG. XXIV. An eccentric Neptune-mass planet near the inner edge of the BD-11 4672 habitable zone.

BARBATO D., PINAMONTI M., SOZZETTI A., BIAZZO K., BENATTI S., DAMASSO M., DESIDERA S., LANZA A.F., MALDONADO J., MANCINI L., SCANDARIATO G., AFFER L., ANDREUZZI G., BIGNAMINI A., BONOMO A.S., BORSA F., CARLEO I., CLAUDI R., COSENTINO R., COVINO E., FIORENZANO A.F.M., GIACOBBE P., HARUTYUNYAN A., KNAPIC C., LETO G., LORENZI V., MAGGIO A., MALAVOLTA L., MICELA G., MOLINARI E., MOLINARO M., NASCIMBENI V., PAGANO I., PEDANI M., PIOTTO G., PORETTI E. and RAINER M.

Abstract (from CDS):


Context. With the growth of comparative exoplanetology, it is becoming increasingly clear that investigating the relationships between inner and outer planets plays a key role in discriminating between competing formation and evolution models. To do so, it is important to probe the inner region of systems that host long-period giants in search of undetected lower-mass planetary companions.
Aims. In this work, we present our results on the K-dwarf star BD-11 4672, which is already known to host a long-period giant planet, as the first output of a subsample of the GAPS programme specifically aimed at assessing the impact of inefficient migration of planets formed beyond the snowline by searching for Neptune-mass and super-Earth planetary companions of known longer-period giants.
Methods. We used the high-precision HARPS-N observations of BD-11 4672 in conjunction with time series taken from the literature in order to search for additional inner planetary signals to be fitted using differential evolution Markov chain Monte Carlo. The long-term stability of the new orbital solutions was tested with N-body dynamical simulations.
Results. We report the detection of BD-11 4672 c, a new Neptune-mass planet with an orbital period of 74.20–0.08+0.06d, eccentricity of 0.40–0.15+0.13, semimajor axis of 0.30±0.01au, and minimum mass 15.37–2.81+2.97M, orbiting slightly outside the inner edge of the optimistic circumstellar habitable zone. In order to assess its impact on the dynamical stability of the habitable zone, we computed the angular momentum deficit of the system, showing that planet c has a severe negative impact on the stability of possible additional lower-mass temperate planets. The BD-11 4672 system is notable for its architecture, hosting both a long-period giant planet and an inner lower-mass planet, the latter being one of the most eccentric Neptune-mass planets known at similar periods.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: individual: BD-11 4672 - techniques: radial velocities - planetary systems - planets and satellites: detection - planets and satellites: dynamical evolution and stability

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 BD+47 612b Pl 02 22 14.6440695182 +47 52 48.110234827           ~ 6 0
2 BD-06 1339 PM* 05 53 00.2845591992 -05 59 41.442052694 12.27 11.041 9.693 8.855 8.099 K7V/M0V 72 1
3 CD-51 10924 PM* 17 30 11.2030058822 -51 38 13.139736838 12.317 11.028 9.585 8.675 8.60 M0V 81 1
4 BD-11 4672b Pl 18 33 28.8322843874 -11 38 09.721813732           ~ 3 0
5 BD-11 4672 PM* 18 33 28.8322843874 -11 38 09.721813732   11.21 9.99 9.60 9.02 K7V 58 1
6 BD-11 4672c Pl? 18 33 28.8322843874 -11 38 09.721813732           ~ 1 0
7 Kepler-278c Pl 19 20 25.7274853511 +38 42 08.031014212           ~ 25 0

    Equat.    Gal    SGal    Ecl

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2020.12.05-00:57:31

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