2014MNRAS.441..442N


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.24CEST02:42:18

2014MNRAS.441..442N - Mon. Not. R. Astron. Soc., 441, 442-451 (2014/June-2)

The 55 Cancri planetary system: fully self-consistent N-body constraints and a dynamical analysis.

NELSON B.E., FORD E.B., WRIGHT J.T., FISCHER D.A., VON BRAUN K., HOWARD A.W., PAYNE M.J. and DINDAR S.

Abstract (from CDS):

We present an updated study of the planets known to orbit 55 Cancri A using 1 418 high-precision radial velocity observations from four observatories (Lick, Keck, Hobby-Eberly Telescope, Harlan J. Smith Telescope) and transit time/durations for the inner-most planet, 55 Cancri `e' (Winn et al.). We provide the first posterior sample for the masses and orbital parameters based on self-consistent N-body orbital solutions for the 55 Cancri planets, all of which are dynamically stable (for at least 108 yr). We apply a GPU version of Radial velocity Using N-body Differential evolution Markov Chain Monte Carlo (run dmc; Nelson, Ford & Payne) to perform a Bayesian analysis of the radial velocity and transit observations. Each of the planets in this remarkable system has unique characteristics. Our investigation of high-cadence radial velocities and priors based on space-based photometry yields an updated mass estimate for planet `e' (8.09±0.26 M), which affects its density (5.51±^1.32_1.00 g/cm3) and inferred bulk composition. Dynamical stability dictates that the orbital plane of planet `e' must be aligned to within 60° of the orbital plane of the outer planets (which we assume to be coplanar). The mutual interactions between the planets `b' and `c' may develop an apsidal lock about 180°. We find 36-45 per cent of all our model systems librate about the anti-aligned configuration with an amplitude of 51^○±^6^○_10^○. Other cases showed short-term perturbations in the libration of πb - πc, circulation, and nodding, but we find the planets are not in a 3:1 mean-motion resonance. A revised orbital period and eccentricity for planet `d' pushes it further towards the closest known Jupiter analogue in the exoplanet population.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): methods: statistical - techniques: radial velocities - planets and satellites: dynamical evolution and stability

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 * rho01 Cnc e Pl 08 52 35.81093 +28 19 50.9511           ~ 355 1
2 * rho01 Cnc d Pl 08 52 35.81093 +28 19 50.9511           ~ 134 1
3 * rho01 Cnc b Pl 08 52 35.81093 +28 19 50.9511     13.16     ~ 224 1
4 * rho01 Cnc f Pl 08 52 35.81093 +28 19 50.9511           ~ 41 1
5 * rho01 Cnc c Pl 08 52 35.81093 +28 19 50.9511           ~ 121 1
6 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 945 1
7 HD 82943 PM* 09 34 50.7352288445 -12 07 46.363303103   7.17 6.53     F9VFe+0.5 395 2
8 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 829 1

    Equat.    Gal    SGal    Ecl

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2019.10.24-02:42:19

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