2022A&A...661A..62A


Query : 2022A&A...661A..62A

2022A&A...661A..62A - Astronomy and Astrophysics, volume 661A, 62-62 (2022/5-1)

Periodic orbits in the 1:2:3 resonant chain and their impact on the orbital dynamics of the Kepler-51 planetary system.

ANTONIADOU K.I. and VOYATZIS G.

Abstract (from CDS):


Aims. Space missions have discovered a large number of exoplanets evolving in (or close to) mean-motion resonances (MMRs) and resonant chains. Often, the published data exhibit very high uncertainties due to the observational limitations that introduce chaos into the evolution of the system on especially shorter or longer timescales. We propose a study of the dynamics of such systems by exploring particular regions in phase space.
Methods. We exemplify our method by studying the long-term orbital stability of the three-planet system Kepler-51 and either favor or constrain its data. It is a dual process which breaks down in two steps: the computation of the families of periodic orbits in the 1:2:3 resonant chain and the visualization of the phase space through maps of dynamical stability.
Results. We present novel results for the general four-body problem. Stable periodic orbits were found only in the low-eccentricity regime. We demonstrate three possible scenarios safeguarding Kepler-51, each followed by constraints. Firstly, there are the 2/1 and 3/2 two-body MMRs, in which eb < 0.02, such that these two-body MMRs last for extended time spans. Secondly, there is the 1:2:3 three-body Laplace-like resonance, in which ec < 0.016 and ed < 0.006 are necessary for such a chain to be viable. Thirdly, there is the combination comprising the 1/1 secondary resonance inside the 2/1 MMR for the inner pair of planets and an apsidal difference oscillation for the outer pair of planets in which the observational eccentricities, eb and ec, are favored as long as ed ~= 0.
Conclusions. With the aim to obtain an optimum deduction of the orbital elements, this study showcases the need for dynamical analyses based on periodic orbits performed in parallel to the fitting processes.

Abstract Copyright: © ESO 2022

Journal keyword(s): celestial mechanics - planets and satellites: dynamical evolution and stability - planetary systems - methods: analytical - methods: numerical - chaos

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 WT 2353 PM* 00 29 12.3029193648 -30 27 13.466857032   13.05 11.95     ~ 61 0
2 K2-32 PM* 16 49 42.2601799152 -19 32 34.151379684   13.28 12.31 12.11   ~ 46 0
3 Kepler-30 Er* 19 01 08.0746104528 +38 56 50.218268856   16.50   15.767 14.55 ~ 152 1
4 Kepler-60 Er* 19 15 50.6983640712 +42 15 54.050260968   14.477 14.083 13.934   G2 107 1
5 Kepler-82 Er* 19 31 29.6083527360 +42 57 58.067640720   15.940 15.318 14.676   ~ 65 1
6 Kepler-47 EB* 19 41 11.4983203032 +46 55 13.707336288           ~ 160 1
7 Kepler-51 Er* 19 45 55.1428629456 +49 56 15.650520684       14.829   G4 124 1
8 Kepler-51d Pl 19 45 55.1428629456 +49 56 15.650520684           ~ 73 0
9 Kepler-51b Pl 19 45 55.1428629456 +49 56 15.650520684           ~ 93 1
10 Kepler-51c Pl 19 45 55.1428629456 +49 56 15.650520684           ~ 50 1
11 Kepler-18 Er* 19 52 19.0688312520 +44 44 46.807928916   14.750 13.767 13.93   ~ 124 1
12 Kepler-223 Er* 19 53 16.4202435936 +47 16 46.308434088   16.209 15.570 15.78   ~ 155 1
13 TRAPPIST-1 LM* 23 06 29.3684948589 -05 02 29.037301866     18.798 16.466 14.024 M7.5e 965 0
14 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1123 0
15 K2-138 * 23 15 47.7686067840 -10 50 58.895461284   13.01 12.21 12.12 11.40 ~ 52 0

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