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 -