2021A&A...646A.148G


Query : 2021A&A...646A.148G

2021A&A...646A.148G - Astronomy and Astrophysics, volume 646A, 148-148 (2021/2-1)

Semianalytical model for planetary resonances. Application to planets around single and binary stars.

GALLARDO T., BEAUGE C. and GIUPPONE C.A.

Abstract (from CDS):


Context. Planetary resonances are a common dynamical mechanism acting on planetary systems. However, no general model for describing their properties exists, particularly for commensurabilities of any order and arbitrary eccentricity and inclination values.
Aims. We present a semianalytical model that describes the resonance strength, width, location and stability of fixed points, and periods of small-amplitude librations. The model is valid for any two gravitationally interacting massive bodies, and is thus applicable to planets around single or binary stars.
Methods. Using a theoretical framework in the Poincare and Jacobi reference system, we developed a semianalytical method that employs a numerical evaluation of the averaged resonant disturbing function. Validations of the model are presented that compare its predictions with dynamical maps for real and fictitious systems.
Results. The model describes many dynamical features of planetary resonances very well. Notwithstanding the good agreement found in all cases, a small deviation is noted in the location of the resonance centers for circumbinary systems. As a consequence of its application to the HD 31527 system, we found that the updated best-fit solution leads to a high-eccentricity stable libration between the middle and outer planets inside the 16/3 mean-motion resonance (MMR). This is the first planetary system whose long-term dynamics appears dominated by such a high-order commensurability. In the case of circumbinary planets, the overlap of N/1 mean-motion resonances coincides very well with the size of the global chaotic region close to the binary, as well as its dependence on the mutual inclination.

Abstract Copyright: © ESO 2021

Journal keyword(s): planets and satellites: dynamical evolution and stability - planets and satellites: individual: HD 31527 - planet-star interactions

Simbad objects: 19

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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 - 2021
#notes
1 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 675 1
2 HD 31527d Pl 04 55 38.3827517884 -23 14 30.758953907           ~ 6 1
3 HD 31527b Pl 04 55 38.3827517884 -23 14 30.758953907           ~ 9 1
4 HD 31527c Pl 04 55 38.3827517884 -23 14 30.758953907           ~ 7 1
5 HD 31527 PM* 04 55 38.3827517884 -23 14 30.758953907   8.071 7.484 7.24 8.88 G0V 79 1
6 TOI-1338 * 06 08 31.9679092936 -59 32 28.080175325   12.537 11.975     ~ 14 0
7 HD 45364 PM* 06 25 38.4744251424 -31 28 51.428476346   8.82 8.06     G8V 108 1
8 HD 74156d Pl? 08 42 25.1221445320 +04 34 41.146391815           ~ 19 1
9 HD 74156b Pl 08 42 25.1221445320 +04 34 41.146391815           ~ 60 1
10 HD 74156c Pl 08 42 25.1221445320 +04 34 41.146391815           ~ 53 1
11 HD 74156 PM* 08 42 25.1221445320 +04 34 41.146391815       7.2   G1V 209 2
12 HD 98800 TT* 11 22 05.28975 -24 46 39.7571   10.20 9.28 9.26 7.386 K5V(e) 343 0
13 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 528 1
14 YLW 15 Y*O 16 27 26.93640 -24 40 50.8224           ~ 246 1
15 * b Her SB* 18 07 01.53971 +30 33 43.6896 5.52 5.59 5.07 4.61 4.28 F7VgF7mF5 425 0
16 Kepler-453 EB* 18 52 57.9087896033 +46 22 42.553490705           G5 60 0
17 Kepler-38 EB* 19 07 19.2813795966 +42 16 45.120332899           ~ 84 1
18 Kepler-47 EB* 19 41 11.4984891255 +46 55 13.705101341           ~ 135 1
19 Kepler-34 EB* 19 45 44.5975310719 +44 38 29.612454271           ~ 133 1

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2021.09.27-17:18:30

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