1,373 research outputs found
Dynamical behaviour of multiplanet systems close to their stability limit
The dynamics of systems of two and three planets, initially placed on
circular and nearly coplanar orbits, is explored in the proximity of their
stability limit. The evolution of a large number of systems is numerically
computed and their dynamical behaviour is investigated with the frequency map
analysis as chaos indicator. Following the guidance of this analysis, it is
found that for two-planet systems the dependence of the Hill limit on the
planet mass, usually made explicit through the Hill's radius parametrization,
does not appear to be fully adequate. In addition, frequent cases of stable
chaos are found in the proximity of the Hill limit. For three-planet systems,
the usual approach adopted in numerical explorations of their stability, where
the planets are initially separated by multiples of the mutual Hill radius,
appears too reducing. A detailed sampling of the parameter space reveals that
systems with more packed inner planets are stable well within previous
estimates of the stability limit. This suggests that a two-dimensional approach
is needed to outline when three-planet systems are dynamically stable.Comment: 7 pages, 3 figures, Accepted on MNRA
The influence of general-relativity effects, dynamical tides and collisions on planet-planet scattering close to the star
Planet--Planet scattering is an efficient and robust dynamical mechanism for
producing eccentric exoplanets. Coupled to tidal interactions with the central
star, it can also explain close--in giant planets on circularized and
potentially misaligned orbits. We explore scattering events occurring close to
the star and test if they can reproduce the main features of the observed
orbital distribution of giant exoplanets on tight orbits.In our modeling we
exploit a numerical integration code based on the Hermite algorithm and
including the effects of general relativity, dynamical tides and two--body
collisions.We find that P--P scattering events occurring in systems with three
giant planets initially moving on circular orbits close to their star produce a
population of planets similar to the presently observed one, including
eccentric and misaligned close--in planets. The contribution of tides and
general relativity is relevant in determining the final outcome of the chaotic
phase. Even if two--body collisions dominate the chaotic evolution of three
planets in crossing orbits close to their star, the final distribution shows a
significant number of planets on eccentric orbits. The highly misaligned
close--in giant planets are instead produced by systems where the initial
semi--major axis of the inner planet was around 0.2 au or beyond.Comment: Accepted for publication on A&
Stability of multiplanet systems in binaries
When exploring the stability of multiplanet systems in binaries, two
parameters are normally exploited: the critical semimajor axis ac computed by
Holman and Wiegert (1999) within which planets are stable against the binary
perturbations, and the Hill stability limit Delta determining the minimum
separation beyond which two planets will avoid mutual close encounters. Our aim
is to test whether these two parameters can be safely applied in multiplanet
systems in binaries or if their predictions fail for particular binary orbital
configurations. We have used the frequency map analysis (FMA) to measure the
diffusion of orbits in the phase space as an indicator of chaotic behaviour.
First we revisited the reliability of the empirical formula computing ac in the
case of single planets in binaries and we find that, in some cases, it
underestimates by 10-20% the real outer limit of stability. For two planet
systems, the value of Delta is close to that computed for planets around single
stars, but the level of chaoticity close to it substantially increases for
smaller semimajor axes and higher eccentricities of the binary orbit. In these
configurations ac also begins to be unreliable and non linear secular
resonances with the stellar companion lead to chaotic behaviour well within ac,
even for single planet systems. For two planet systems, the superposition of
mean motion resonances, either mutual or with the binary companion, and non
linear secular resonances may lead to chaotic behaviour in all cases. We have
developed a parametric semiempirical formula determining the minimum value of
the binary semimajor axis, for a given eccentricity of the binary orbit, below
which stable two planet systems cannot exist.Comment: Accepted on A&
Dynamics of Jupiter Trojans during the 2:1 mean motion resonance crossing of Jupiter and Saturn
We study the dynamics of Jupiter Trojans in the early phase of the Solar
system while the outer planets migrated due to their interaction with the
planetesimal disk.Comment: 10 pages, 17 figure
Planet--planet scattering in circumstellar gas disks
Hydrodynamical simulations of two giant planets embedded in a gaseous disk
have shown that in case of a smooth convergent migration they end up trapped
into a mean motion resonance. These findings have led to the conviction that
the onset of dynamical instability causing close encounters between the planets
can occur only after the dissipation of the gas when the eccentricity damping
is over. We show that a system of three giant planets may undergo planet-planet
scattering when the gaseous disk, with density values comparable to that of the
Minimum Mass Solar Nebula, is still interacting with the planets. The
hydrodynamical code FARGO--2D--1D is used to model the evolution ofthe disk and
planets, modified to properly handle close encounters between the massive
bodies. Our simulations predict a variety of different outcomes of the
scattering phase which includes orbital exchange, planet merging and scattering
of a planet in a hyperbolic orbit. This implies thatthe final fate of a
multiplanet system under the action of the disk torques is not necessarily a
packed resonant configuration.Comment: Astronomy and Astrophysics Letters, in pres
Planets in binary systems: is the present configuration indicative of the formation process?
The present dynamical configuration of planets in binary star systems may not
reflect their formation process since the binary orbit may have changed in the
past after the planet formation process was completed. An observed binary
system may have been part of a former hierarchical triple that became unstable
after the planets completed their growth around the primary star.
Alternatively, in a dense stellar environment even a single stellar encounter
between the star pair and a singleton may singificantly alter the binary orbit.
In both cases the planets we observe at present would have formed when the
dynamical environment was different from the presently observed one.
We have numerically integrated the trajectories of the stars (binary plus
singleton) and of test planets to investigate the abovementioned mechanisms.
Our simulations show that the circumstellar environment during planetary
formation around the primary was gravitationally less perturbed when the binary
was part of a hierarchical triple because the binary was necessarely wider and,
possibly, less eccentric. This circumstance has consequences for the planetary
system in terms of orbital spacing, eccentricity, and mass of the individual
planets. Even in the case of a single stellar encounter the present appearance
of a planetary system in a binary may significantly differ from what it had
while planet formation was ongoing. However, while in the case of instability
of a triple the trend is always towards a tighter and more eccentric binary
system, when a single stellar encounter affects the system the orbit of the
binary can become wider and be circularized.Comment: 5 pages, 5 figures Accepted for publication on A&
Dust-to-gas ratio resurgence in circumstellar disks due to the formation of giant planets: the case of HD 163296
The amount of dust present in circumstellar disks is expected to steadily
decrease with age due to the growth from micron-sized particles to
planetesimals and planets. Mature circumstellar disks, however, can be observed
to contain significant amounts of dust and possess high dust-to-gas ratios.
Using HD 163296 as our case study, we explore how the formation of giant
planets in disks can create the conditions for collisionally rejuvenating the
dust population, halting or reversing the expected trend. We combine N-body
simulations with statistical methods and impact scaling laws to estimate the
dynamical and collisional excitation of the planetesimals due to the formation
of HD 163296's giant planets. We show that this process creates a violent
collisional environment across the disk that can inject collisionally produced
second-generation dust into it, significantly contributing to the observed
dust-to-gas ratio. The spatial distribution of the dust production can explain
the observed local enrichments in HD 163296's inner regions. The results
obtained for HD 163296 can be extended to any disk with embedded forming giant
planets and may indicate a common evolutionary stage in the life of such
circumstellar disks. Furthermore, the dynamical excitation of the planetesimals
could result in the release of transient, non-equilibrium gas species like H2O,
CO2, NH3 and CO in the disk due to ice sublimation during impacts and, due to
the excited planetesimals being supersonic with respect to the gas, could
produce bow shocks in the latter that could heat it and cause a broadening of
its emission lines.Comment: 18 pages, 9 figures, 2 tables. Accepted for publication on The
Astrophysical Journa
Asteroid detection at millimetric wavelengths with the Planck survey
The Planck mission, originally devised for cosmological studies, offers the
opportunity to observe Solar System objects at millimetric and submillimetric
wavelengths. We concentrate in this paper on the asteroids of the Main Belt. We
intend to estimate the number of asteroids that can can be detected during the
mission and to evaluate the strength of their signal. We have rescaled the
instrument sensitivities, calculated by the LFI and HFI teams for sources fixed
in the sky, introducing some degradation factors to properly account for moving
objects. In this way a detection threshold is derived for asteroidal detection
that is related to the diameter of the asteroid and its geocentric distance. We
have developed a numerical code that models the detection of asteroids in the
LFI and HFI channels during the mission. This code perfoprms a detailed
integration of the orbits of the asteroids in the timespan of the mission and
identifies those bodies that fall in the beams of Planck and their signal
stenght. According to our simulations, a total of 397 objects will be observed
by Planck and an asteroidal body will be detected in some beam in 30% of the
total sky scan--circles. A significant fraction (in the range from ~50 to 100
objects) of the 397 asteroids will be observed with a high S/N ratio. Flux
measurements of a large sample of asteroids in the submillimeter and millimeter
range are relevant since they allow to analyze the thermal emission and its
relation to the surface and regolith properties. Furthermore, it will be
possible to check on a wider base the two standard thermal models, based on a
nonrotating or rapidly rotating sphere. Our method can also be used to separate
Solar System sources from cosmological sources in the survey. This work is
based on Planck LFI activities.Comment: Contact person [email protected]. Accepted for pubblication in
New Astronomy (2002). 1 figure in .eps format. Needs elsart.cls style +
harvard.st
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