41,655 research outputs found
Corrections to scaling in the dynamic approach to the phase transition with quenched disorder
With dynamic Monte Carlo simulations, we investigate the continuous phase
transition in the three-dimensional three-state random-bond Potts model. We
propose a useful technique to deal with the strong corrections to the dynamic
scaling form. The critical point, static exponents and , and
dynamic exponent are accurately determined. Particularly, the results
support that the exponent satisfies the lower bound .Comment: 10 pages, 6 figures, 2 table
Dynamic effect of overhangs and islands at the depinning transition in two-dimensional magnets
With the Monte Carlo methods, we systematically investigate the short-time
dynamics of domain-wall motion in the two-dimensional random-field Ising model
with a driving field ?DRFIM?. We accurately determine the depinning transition
field and critical exponents. Through two different definitions of the domain
interface, we examine the dynamics of overhangs and islands. At the depinning
transition, the dynamic effect of overhangs and islands reaches maximum. We
argue that this should be an important mechanism leading the DRFIM model to a
different universality class from the Edwards-Wilkinson equation with quenched
disorderComment: 9 pages, 6 figure
The dynamical fate of planetary systems in young star clusters
We carry out N-body simulations to examine the effects of dynamical
interactions on planetary systems in young open star clusters. We explore how
the planetary populations in these star clusters evolve, and how this evolution
depends on the initial amount of substructure, the virial ratio, the cluster
mass and density, and the initial semi-major axis of the planetary systems. The
fraction of planetary systems that remains intact as a cluster member, fbps, is
generally well-described by the functional form fbps=f0(1+[a/a0]^c)^-1, where
(1-f0) is the fraction of stars that escapes from the cluster, a0 the critical
semi-major axis for survival, and c a measure for the width of the transition
region. The effect of the initial amount of substructure over time can be
quantified as fbps=A(t)+B(D), where A(t) decreases nearly linearly with time,
and B(D) decreases when the clusters are initially more substructured. Provided
that the orbital separation of planetary systems is smaller than the critical
value a0, those in clusters with a higher initial stellar density (but
identical mass) have a larger probability of escaping the cluster intact. These
results help us to obtain a better understanding of the difference between the
observed fractions of exoplanets-hosting stars in star clusters and in the
Galactic field. It also allows us to make predictions about the free-floating
planet population over time in different stellar environments.Comment: 14 pages, 9 figures, accepted for publication in MNRA
Critical domain-wall dynamics of model B
With Monte Carlo methods, we simulate the critical domain-wall dynamics of
model B, taking the two-dimensional Ising model as an example. In the
macroscopic short-time regime, a dynamic scaling form is revealed. Due to the
existence of the quasi-random walkers, the magnetization shows intrinsic
dependence on the lattice size . A new exponent which governs the
-dependence of the magnetization is measured to be .Comment: 10pages, 4 figure
Clearing residual planetesimals by sweeping secular resonances in transitional disks: a lone-planet scenario for the wide gaps in debris disks around Vega and Fomalhaut
Extended gaps in the debris disks of both Vega and Fomalhaut have been
observed. These structures have been attributed to tidal perturbations by
multiple super-Jupiter gas giant planets. Within the current observational
limits, however, no such massive planets have been detected. Here we propose a
less stringent `lone-planet' scenario to account for the observed structure
with a single eccentric gas giant and suggest that clearing of these wide gaps
is induced by its sweeping secular resonance. During the depletion of the disk
gas, the planet's secular resonance propagates inward and clears a wide gap
over an extended region of the disk. Although some residual intermediate-size
planetesimals may remain in the gap, their surface density is too low to either
produce super-Earths or lead to sufficiently frequent disruptive collisions to
generate any observable dusty signatures. The main advantage of this
lone-planet sweeping-secular-resonance model over the previous multiple gas
giant tidal truncation scenario is the relaxed requirement on the number of gas
giants. The observationally inferred upper mass limit can also be satisfied
provided the hypothetical planet has a significant eccentricity. A significant
fraction of solar or more massive stars bear gas giant planets with significant
eccentricities. If these planets acquired their present-day kinematic
properties prior to the depletion of their natal disks, their sweeping secular
resonance would effectively impede the retention of neighboring planets and
planetesimals over a wide range of orbital semi-major axes.Comment: 20 pages, 12 figures. Accepted for publication in Ap
Close encounters involving free-floating planets in star clusters
Instabilities in planetary systems can result in the ejection of planets from
their host system, resulting in free-floating planets (FFPs). If this occurs in
a star cluster, the FFP may remain bound to the star cluster for some time and
interact with the other cluster members until it is ejected. Here, we use
-body simulations to characterise close star-planet and planet-planet
encounters and the dynamical fate of the FFP population in star clusters
containing single or binary star members. We find that FFPs ejected
from their planetary system at low velocities typically leave the star cluster
40% earlier than their host stars, and experience tens of close ( AU)
encounters with other stars and planets before they escape. The fraction of
FFPs that experiences a close encounter depends on both the stellar density and
the initial velocity distribution of the FFPs. Approximately half of the close
encounters occur within the first 30 Myr, and only 10% occur after 100 Myr. The
periastron velocity distribution for all encounters is well-described by a
modified Maxwell-Bolzmann distribution, and the periastron distance
distribution is linear over almost the entire range of distances considered,
and flattens off for very close encounters due to strong gravitational
focusing. Close encounters with FFPs can perturb existing planetary systems and
their debris structures, and they can result in re-capture of FFPs. In
addition, these FFP populations may be observed in young star clusters in
imaging surveys; a comparison between observations and dynamical predictions
may provide clues to the early phases of stellar and planetary dynamics in star
clusters.Comment: Accepted for publication in MNRAS; 18 pages, 12 figure
Relaxation-to-creep transition of domain-wall motion in two- dimensional random-field Ising model with ac driving field
With Monte Carlo simulations, we investigate the relaxation dynamics with a
domain wall for magnetic systems at the critical temperature. The dynamic
scaling behavior is carefully analyzed, and a dynamic roughening process is
observed. For comparison, similar analysis is applied to the relaxation
dynamics with a free or disordered surfaceComment: 5 pages, 5 figure
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