Doppler and transit observations of exoplanets show a pile-up Jupiter-size planets in orbits with 3 day period. A fraction these hot Jupiters have retrograde respect to the parent star's rotation, as evidenced by measurements Rossiter–McLaughlin effect. To explain we performed series numerical integrations planet scattering followed tidal circularization migration that evolved into highly eccentric orbits. We considered planetary systems having three four initially placed successive...

We analyze the distribution of extrasolar planets (both confirmed and Kepler candidates) according to their orbital periods P planetary radii R. Among planets, we find compelling evidence for a paucity bodies with 3 < R 10 R_\oplus, where R_\oplus in Earth's radius, 2-3 days. have christened this region "sub-Jovian Pampas". The same trend is detected multiplanet candidates. Although approximately 16 single-planet candidates inhabit Pampas, at least 7 are probable false positives (FP). This...

In this paper, we present a new set of corotational solutions for the 2/1 commensurability, including previously known and results. Comparisons with observed exoplanets show that current orbital fits three proposed resonant planetary systems are consistent apsidal corotations.

In recent years several pairs of extrasolar planets have been discovered in the vicinity mean-motion commensurabilities. some cases, such as Gliese 876 system, seem to be trapped a stationary solution, system exhibiting simultaneous libration resonant angle theta_1 = 2 lambda_2 - lambda_1 varpi_1 and relative position pericenters. this paper we analyze existence location these stable solutions, for 2/1 3/1 resonances, function masses orbital elements both planets. This is undertaken via an...

The lower limit to the distribution of orbital periods P for current population close-in exoplanets shows a distinctive discontinuity located at approximately one Jovian mass. Most smaller planets have longer than P~2.5 days, while higher masses are found down P~1 day. We analyze whether this observed mass-period could be explained in terms combined effects stellar tides and interactions with an inner cavity gaseous disk. performed series hydrodynamical simulations evolution single-planet...

Aims.We study the formation of a hypothetical terrestrial-type body in equilateral Lagrange points giant extrasolar planet. Starting from swarm planetesimals stable tadpole orbits, we simulate its dynamical and collisional evolution under wide range different initial conditions masses for both Trojan population planetary companion. We also analyze effects gas drag interaction with nebular disk.

We analyse the global structure of phase space planar planetary 2/1 mean-motion resonance in cases where outer planet is more massive than its inner companion. Inside resonant domain, we show existence two families periodic orbits, one associated to librational motion angle (σ-family) and other related circulatory difference longitudes pericentre (Δϖ-family). The well-known apsidal corotation resonances (ACR) appear as intersections between both families. A complex web secondary also...

We study the stability regions and families of periodic orbits two planets locked in a co-orbital configuration. consider different ratios planetary masses orbital eccentricities, also we assume that both share same plane. Initially perform numerical simulations over grid osculating initial conditions to map stable/chaotic motion identify equilibrium solutions. These results are later analyzed more detail using semi-analytical model. Apart from well known quasi-satellite (QS) classical...

This investigation uses the excellent HARPS radial velocity measurements of CoRoT-7 to re-determine planet masses and explore techniques able determine mass elements planets discovered around active stars when relative variation due star activity cannot be considered as just noise can exceed planets. The main technique used here is a self-consistent version high-pass filter by Queloz et al. (2009) in first determination CoRoT-7b CoRoT-7c. results are compared those given two alternative...

The existence of multiple planetary systems involved in mean motion conmensurabilities has increased significantly since the Kepler mission. Although most correspond to 2-planet resonances, resonances have also been found. Laplace resonance is a particular case three-body where period ratio between consecutive pairs n_1/n_2 near n_2/n_3 2/1. It not clear how this triple can act order stabilize (or not) systems. reliable extrasolar system located GJ876 because it two independent...

Chaotic diffusion is supposed to be responsible for orbital instabilities in planetary systems after the dissipation of protoplanetary disk, and a natural consequence irregular motion. In this paper we show that resonant multi-planetary systems, despite being highly chaotic, not necessarily exhibit significant phase space, may still survive virtually unchanged over timescales comparable their age.Using GJ-876 system as an example, analyze chaotic outermost (and less massive) planet. We...

As the Galactic tide acts to decouple bodies from scattered disk it creates a spiral structure in physical space that is roughly 15,000 au length. The long-lived and persists inner Oort cloud present time. Here we discuss dynamics underlying (feeble) prospects for its observational detection.

The discovery of extrasolar planets located in the vicinity mean-motion commensurabilities has opened a new arena for study resonance capture and its possible role dynamical evolution long-term stability planetary systems. Contrary to our own Solar System, many these have highly eccentric orbits (∼0.1–0.6), making use usual analytical perturbative models very limited. Even so, several attempts been made apply classical expansions resonant Hamiltonian cases, leading results which are, at...

The published orbits of the planets HD 82943b and 82943c correspond to a system bound catastrophic event in less than 100,000 years. Alternative sets elements masses, which fit available observational data regular motions, are presented this paper. 82943 c,b 2/1 mean-motion resonance trapped neighborhood (0,0)-apsidal corotation.

We perform a statistical study of the process orbital determination HD82943 extrasolar planetary system, using current observational data set N= 165 radial velocity (RV) measurements. Our aim is to analyse dispersion possible fits leading residuals compatible with best solution, and discuss sensitivity results respect both error distribution around fit. Although some parameters (e.g. semimajor axis) appear well constrained, we show that for system are not robust, at present it estimate...

We analyse the possibilities of detection hypothetical exoplanets in co-orbital motion from synthetic radial velocity (RV) signals, taking into account different types stable planar configurations, orbital eccentricities and mass ratios. For each nominal solution corresponding to small-amplitude oscillations around periodic solution, we generate a series RV curves mimicking stellar barycentre system. then fit data sets obtained assuming three possible architectures: (a) two planets motion,...

We present a new method that allows long-term and large-scale hydrodynamical simulations of migrating planets over grid-based Eulerian code. This technique, which consists in remapping the disk by tracking planetary migration, enables runs time comparable to age protoplanetary disks. also has potential address efficiently problems related with migration multi-planet systems gaseous disks, improve current results massive including global viscous evolution as well detailed studies co-orbital...

This paper presents the second part in our study of global structure planar phase space planetary three-body problem, when both planets lie vicinity a 2/1 mean-motion resonance. While Paper I was devoted to cases where outer planet is more massive body, present work body inner planet. As before, outside well-known Apsidal Corotation Resonances (ACR), shows complex picture marked by presence several distinct regimes resonant and non-resonant motion, crossed families periodic orbits separated...

The Transit Timing Variation (TTV) method relies on monitoring changes in timing of transits known exoplanets. Non-transiting planets the system can be inferred from TTVs by their gravitational interaction with transiting planet. TTV is sensitive to low-mass that cannot detected other means. Here we describe a fast algorithm used determine mass and orbit non-transiting data. We apply our code, ttvim.f, wide variety planetary systems test uniqueness inversion problem its dependence precision...