2013A&A...560A..65C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST09:19:29

2013A&A...560A..65C - Astronomy and Astrophysics, volume 560A, 65-65 (2013/12-1)

A new scenario for the origin of the 3/2 resonant system HD 45364.

CORREA-OTTO J.A., MICHTCHENKO T.A. and BEAUGE C.

Abstract (from CDS):

We revise the model for the origin of the HD45364 exoplanetary system proposed by Rein et al. (2010A&A...510A...4R), which is currently known to host two planets close to the 3/2 mean-motion resonance (MMR). We show that due to the high surface density of the protoplanetary disk needed for type III migration, this model can only lead to planets in a quasi-resonant regime of motion and thus is not consistent with the resonant configuration obtained by Correia et al. (2009A&A...496..521C). Although both resonant and quasi-resonant solutions are statistically indistinguishable with respect to radial velocity measurements, their distinct dynamical behavior is intriguing. We used the semi-analytical model to confirm the quantitative difference between two configurations. To form a system that evolves inside the 3/2 resonance, we developed a different model. Our scenario includes an interaction between different (but slower) planetary migration types, planet growth, and gap formation in the protoplanetary disk. The evolutionary path was chosen due to a detailed analysis of the phase space structure in the vicinity of the 3/2 MMR that employed dynamical mapping techniques. The outcomes of our simulations are able to very closely reproduce the 3/2 resonant dynamics obtained from the best fit presented by Correia et al. (2009A&A...496..521C). In addition, by varying the strength of the eccentricity damping, we can also simulate the quasi-resonant configuration similar to that reported in Rein et al. (2010A&A...510A...4R). We furthermore show that our scenario is reliable with respect to the physical parameters involved in the resonance-trapping process. However, our scenario can only be confirmed with additional radial velocities measurements.

Abstract Copyright:

Journal keyword(s): celestial mechanics - planets and satellites: formation - planets and satellites: dynamical evolution and stability - methods: numerical

Simbad objects: 4

goto Full paper

goto View the reference in ADS

Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 45364 PM* 06 25 38.4744251424 -31 28 51.428476346   8.82 8.06     G8V 98 1
2 HD 45364c Pl 06 25 38.4744251424 -31 28 51.428476346           ~ 20 1
3 HD 45364b Pl 06 25 38.4744251424 -31 28 51.428476346           ~ 18 1
4 HD 204313 PM* 21 28 12.2060697389 -21 43 34.516646513   8.696 8.02 7.76   G5V 82 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2013A&A...560A..65C and select 'bookmark this link' or equivalent in the popup menu


2020.07.12-09:19:29

© Université de Strasbourg/CNRS

    • Contact