2008A&A...482..665G


Query : 2008A&A...482..665G

2008A&A...482..665G - Astronomy and Astrophysics, volume 482, 665-672 (2008/5-1)

Are retrograde resonances possible in multi-planet systems?

GAYON J. and BOIS E.

Abstract (from CDS):

Most multi-planetary systems are characterized by hot-Jupiters close to their central star, moving on eccentric orbits. From a dynamical point of view, compact multi-planetary systems form a specific class of the general N-body problem (where N≥3). Moreover, extrasolar planets are found in prograde orbits about their host star, and often in mean motion resonances (MMR). In a first step, we study theoretically a new stabilizing mechanism suitable for compact two-planet systems. This mechanism involves counter-revolving orbits forming a retrograde MMR. In a second step, we investigate the feasibility of planetary systems hosting counter-revolving planets. Dynamical stability, observations, and formation processes of these systems are analyzed and discussed. To characterize the dynamical behavior of multi-dimensional planetary systems, we apply our technique of global dynamics analysis based on the MEGNO indicator (Mean Exponential Growth factor of Nearby Orbits) that provides the fine structure of the phase space. In a few cases of possible counter-revolving configurations, we carry out new fits to the observations using the Pikaia genetic algorithm. A statistical study of the stability in the neighborhood of different observed, planetary-systems is completed using a Monte-Carlo method. We analyse the observational data for the HD 73526 planetary system and find that counter-revolving configurations may be consistent with the observational data. We highlight the fine and characteristic structure of retrograde MMRs. We demonstrate that retrograde resonances open a family of stabilizing mechanisms involving new apsidal precession behaviors. Considering two possible formation mechanisms (free-floating planet and Slingshot model), we conclude that counter-revolving configurations are feasible.

Abstract Copyright:

Journal keyword(s): celestial mechanics - stars: planetary systems - methods: numerical

Simbad objects: 19

goto Full paper

goto View the references in ADS

Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * ups And PM* 01 36 47.8415443907 +41 24 19.651368029 4.70 4.64 4.10 3.64 3.35 F9V 917 1
2 HD 12661 PM* 02 04 34.2881404104 +25 24 51.513637932   8.16   7.0   K0V 244 1
3 HD 37124 PM* 05 37 02.4866159419 +20 43 50.832948117   8.35   7.2   G4IV-V 280 2
4 HD 38529 PM* 05 46 34.9131388488 +01 10 05.502949860       5.4   G8III/IV 329 2
5 HD 69830 PM* 08 18 23.9469682407 -12 37 55.817187530   6.74 5.95     G8:V 494 1
6 HD 73526 PM* 08 37 16.4833548528 -41 19 08.790456324   9.69 9.00     G6V 177 2
7 HD 73526b Pl 08 37 16.4834968915 -41 19 08.787335986           ~ 48 1
8 HD 73526c Pl 08 37 16.4834968915 -41 19 08.787335986           ~ 38 1
9 * rho01 Cnc PM* 08 52 35.8111044043 +28 19 50.954994470 7.45 6.82   5.4   K0IV-V 1036 1
10 HD 82943 PM* 09 34 50.7353072232 -12 07 46.369202196   7.17 6.53     F9VFe+0.5 432 2
11 * 47 UMa PM* 10 59 27.9727514012 +40 25 48.920572724   5.66   4.7   G1-VFe-0.5 746 1
12 HD 108874 PM* 12 30 26.8817398344 +22 52 47.377485192   9.49   8.3   G9V 148 1
13 HD 128311 BY* 14 36 00.5602765558 +09 44 47.454573266 9.232 8.441 7.446 6.895 6.425 K3V 287 1
14 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 587 2
15 * mu. Ara PM* 17 44 08.7031414872 -51 50 02.591603160   5.85 5.15     G3IV-V 497 2
16 * mu. Ara c Pl 17 44 08.7036342277 -51 50 02.591049123           ~ 79 2
17 * mu. Ara b Pl 17 44 08.7036342277 -51 50 02.591049123           ~ 81 2
18 HD 202206 PM* 21 14 57.7686051936 -20 47 21.161521320   8.79 8.07     G6V 210 1
19 BD-15 6290 BY* 22 53 16.7325836486 -14 15 49.304052185 12.928 11.749 10.192 9.013 7.462 M3.5V 922 1

To bookmark this query, right click on this link: simbad:objects in 2008A&A...482..665G and select 'bookmark this link' or equivalent in the popup menu


2022.05.27-05:37:20

© Université de Strasbourg/CNRS

    • Contact