TY - JOUR AU - Crida, A AU - Sándor, Zsolt AU - Kley, W TI - Influence of an inner disc on the orbital evolution of massive planets migrating in resonance JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 483 PY - 2008 SP - 325 EP - 337 PG - 13 SN - 0004-6361 DO - 10.1051/0004-6361:20079291 UR - https://m2.mtmt.hu/api/publication/2794761 ID - 2794761 N1 - Cited By :81 Export Date: 5 January 2023 CODEN: AAEJA Correspondence Address: Crida, A.; Institut für Astronomie and Astrophysik, Auf der Morgenstelle 10, 72076 Tübingen, Germany; email: crida@tat.physik.uni-tuebingen.de AB - Context: The formation of resonant planet pairs in exoplanetary systems involves planetary migration inside the protoplanetary disc. After a resonant capture, subsequent migration leads to a large increase in planetary eccentricities, if no damping mechanism is applied. This has led to the conclusion that the migration of resonant planetary systems cannot take place across large radial distances, but must be terminated rapidly by disc dissipation.
Aims: We investigate if the presence of an inner disc could supply eccentricity damping to the inner planet, and if this effect could explain observed eccentricities in some planetary systems.
Methods: We compute hydrodynamic simulations of giant planets, in orbits of a given eccentricity about an inner gas disc, and measure the effect of the gas disc on the planetary orbital parameters. We perform detailed long-term calculations of the GJ 876 system. We complete N-body simulations, which include artificial forces on the planets that recreate the effect of the inner and outer discs.
Results: We find that we cannot neglect the influence of the inner disc, and that the disc could explain the observed eccentricities. In particular, we reproduce the orbital parameters of a few systems engaged in 2:1 mean motion resonances: GJ 876, HD 73 526, HD 82 943, and HD 128 311. Analytically, we derive the effect that the inner disc should have on the inner planet to reach a specific orbital configuration, for any given damping effect of the outer disc on the outer planet.
Conclusions: We conclude that an inner disc, even though difficult to model properly in hydrodynamical simulations, should be taken into account because of its damping effect on the eccentricity of the inner planet. By including this effect, we can explain quite naturally the observed orbital elements of the pairs of known resonant exoplanets. LA - English DB - MTMT ER - TY - JOUR AU - Érdi, Bálint AU - Nagy, Imre AU - Sándor, Zsolt AU - Süli, Áron AU - Fröhlich, Georgina TI - Secondary resonances of co-orbital motions JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 381 PY - 2007 IS - 1 SP - 33 EP - 40 PG - 8 SN - 0035-8711 DO - 10.1111/j.1365-2966.2007.12228.x UR - https://m2.mtmt.hu/api/publication/1457216 ID - 1457216 AB - The size distribution of the stability region around the Lagrangian point L-4 is investigated in the elliptic restricted three-body problem as the function of the mass parameter and the orbital eccentricity of the primaries. It is shown that there are minimum zones in the size distribution of the stability regions, and these zones are connected with the secondary resonances between the frequencies of librational motions around L-4. The results can be applied to hypothetical Trojan planets for predicting values of the mass parameter and the eccentricity for which such objects can be expected or their existence is less probable. LA - English DB - MTMT ER - TY - JOUR AU - Sándor, Zsolt AU - Kley, W AU - Klagyivik, Péter TI - Stability and formation of the resonant system HD 73526 JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 472 PY - 2007 IS - 3 SP - 981 EP - 992 PG - 12 SN - 0004-6361 DO - 10.1051/0004-6361:20077345 UR - https://m2.mtmt.hu/api/publication/2214221 ID - 2214221 LA - English DB - MTMT ER - TY - JOUR AU - Sándor, Zsolt AU - Kley, W TI - On the evolution of the resonant planetary system HD 128311 JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 451 PY - 2006 SP - L31 EP - L34 SN - 0004-6361 DO - 10.1051/0004-6361:20065196 UR - https://m2.mtmt.hu/api/publication/2794764 ID - 2794764 AB - Context.A significant number of the known multiple exoplanetary systems contain a pair of giant planets engaged in low-order mean-motion resonance. Such a resonant condition protects the dynamics of these planets resulting in very stable orbits. According to recent studies, this capture into a resonance is the result of a planetary migration process induced by interaction of the planets with a protoplanetary disk. If the migration is slow enough (adiabatic) near a mean motion resonance, the two planets will also be in apsidal corotation.
Aims.The recently refined orbital parameters of the system HD 128311 suggest that the two giant planets are in a 2:1 mean motion resonance, however, without exhibiting apsidal corotation. Thus the evolution of this system cannot be described by an adiabatic migration process alone. We present possible evolution scenarios of this system by combining migration processes and sudden perturbations.
Methods.We model migration scenarios through numerical integration of the gravitational N-body problem with additional non-conservative forces. Planet-planet scattering has been investigated by N-body simulations.
Results.We show that the present dynamical state of the system HD 128311 may be explained by such evolutionary processes.
LA - English DB - MTMT ER -