268 research outputs found
Inventory of streams on Theodore Roosevelt Memorial Ranch Dupuyer Montana : implications for livestock grazing and ranch management
Bondi-Hoyle-Lyttleton Accretion onto a Protoplanetary Disk
Young stellar systems orbiting in the potential of their birth cluster can
accrete from the dense molecular interstellar medium during the period between
the star's birth and the dispersal of the cluster's gas. Over this time, which
may span several Myr, the amount of material accreted can rival the amount in
the initial protoplanetary disk; the potential importance of this `tail-end'
accretion for planet formation was recently highlighted by Throop & Bally
(2008). While accretion onto a point mass is successfully modeled by the
classical Bondi-Hoyle-Lyttleton solutions, the more complicated case of
accretion onto a star-disk system defies analytic solution. In this paper we
investigate via direct hydrodynamic simulations the accretion of dense
interstellar material onto a star with an associated gaseous protoplanetary
disk. We discuss the changes to the structure of the accretion flow caused by
the disk, and vice versa. We find that immersion in a dense accretion flow can
redistribute disk material such that outer disk migrates inwards, increasing
the inner disk surface density and reducing the outer radius. The accretion
flow also triggers the development of spiral density features, and changes to
the disk inclination. The mean accretion rate onto the star remains roughly the
same with and without the presence of a disk. We discuss the potential impact
of this process on planet formation, including the possibility of triggered
gravitational instability; inclination differences between the disk and the
star; and the appearance of spiral structure in a gravitationally stable
system.Comment: Accepted to ApJ. Version 2 replaces a mislabeled figure. Animations
of the simulations and a version of the paper with slightly less-compressed
images can be found at http://origins.colorado.edu/~moeckel/BHLpape
Exact results for nonlinear ac-transport through a resonant level model
We obtain exact results for the transport through a resonant level model
(noninteracting Anderson impurity model) for rectangular voltage bias as a
function of time. We study both the transient behavior after switching on the
tunneling at time t = 0 and the ensuing steady state behavior. Explicit
expressions are obtained for the ac-current in the linear response regime and
beyond for large voltage bias. Among other effects, we observe current ringing
and PAT (photon assisted tunneling) oscillations.Comment: 7 page
Contribution of a time-dependent metric on the dynamics of an interface between two immiscible electro-magnetically controllable Fluids
We consider the case of a deformable material interface between two
immiscible moving media, both of them being magnetiable. The time dependence of
the metric at the interface introduces a non linear term, proportional to the
mean curvature, in the surface dynamical equations of mass momentum and angular
momentum. We take into account the effects of that term also in the singular
magnetic and electric fields inside the interface which lead to the existence
of currents and charges densities through the interface, from the derivation of
the Maxwell equations inside both bulks and the interface. Also, we give the
expression for the entropy production and of the different thermo-dynamical
fluxes. Our results enlarge previous results from other theories where the
specific role of the time dependent surface metric was insufficiently stressed.Comment: 25 page
Chaos in black holes surrounded by gravitational waves
The occurrence of chaos for test particles moving around Schwarzschild black
holes perturbed by a special class of gravitational waves is studied in the
context of the Melnikov method. The explicit integration of the equations of
motion for the homoclinic orbit is used to reduce the application of this
method to the study of simple graphics.Comment: 15 pages, LaTex
Stellar Encounters with Massive Star-Disk Systems
The dense, clustered environment in which massive stars form can lead to
interactions with neighboring stars. It has been hypothesized that collisions
and mergers may contribute to the growth of the most massive stars. In this
paper we extend the study of star-disk interactions to explore encounters
between a massive protostar and a less massive cluster sibling using the
publicly available SPH code GADGET-2. Collisions do not occur in the parameter
space studied, but the end state of many encounters is an eccentric binary with
a semi-major axis ~ 100 AU. Disk material is sometimes captured by the
impactor. Most encounters result in disruption and destruction of the initial
disk, and periodic torquing of the remnant disk. We consider the effect of the
changing orientation of the disk on an accretion driven jet, and the evolution
of the systems in the presence of on-going accretion from the parent core.Comment: 11 pages, 10 figures, accepted to Ap
Many-body localization and thermalization in the full probability distribution function of observables
We investigate the relation between thermalization following a quantum quench
and many-body localization in quasiparticle space in terms of the long-time
full distribution function of physical observables. In particular, expanding on
our recent work [E. Canovi {\em et al.}, Phys. Rev. B {\bf 83}, 094431 (2011)],
we focus on the long-time behavior of an integrable XXZ chain subject to an
integrability-breaking perturbation. After a characterization of the breaking
of integrability and the associated localization/delocalization transition
using the level spacing statistics and the properties of the eigenstates, we
study the effect of integrability-breaking on the asymptotic state after a
quantum quench of the anisotropy parameter, looking at the behavior of the full
probability distribution of the transverse and longitudinal magnetization of a
subsystem. We compare the resulting distributions with those obtained in
equilibrium at an effective temperature set by the initial energy. We find
that, while the long time distribution functions appear to always agree {\it
qualitatively} with the equilibrium ones, {\it quantitative} agreement is
obtained only when integrability is fully broken and the relevant eigenstates
are diffusive in quasi-particle space.Comment: 18 pages, 11 figure
Molecular MR Imaging of Prostate Cancer
This review summarizes recent developments regarding molecular imaging markers for magnetic resonance imaging (MRI) of prostate cancer (PCa). Currently, the clinical standard includes MR imaging using unspecific gadolinium-based contrast agents. Specific molecular probes for the diagnosis of PCa could improve the molecular characterization of the tumor in a non-invasive examination. Furthermore, molecular probes could enable targeted therapies to suppress tumor growth or reduce the tumor size
Near-adiabatic parameter changes in correlated systems: Influence of the ramp protocol on the excitation energy
We study the excitation energy for slow changes of the hopping parameter in
the Falicov-Kimball model with nonequilibrium dynamical mean-field theory. The
excitation energy vanishes algebraically for long ramp times with an exponent
that depends on whether the ramp takes place within the metallic phase, within
the insulating phase, or across the Mott transition line. For ramps within
metallic or insulating phase the exponents are in agreement with a perturbative
analysis for small ramps. The perturbative expression quite generally shows
that the exponent depends explicitly on the spectrum of the system in the
initial state and on the smoothness of the ramp protocol. This explains the
qualitatively different behavior of gapless (e.g., metallic) and gapped (e.g.,
Mott insulating) systems. For gapped systems the asymptotic behavior of the
excitation energy depends only on the ramp protocol and its decay becomes
faster for smoother ramps. For gapless systems and sufficiently smooth ramps
the asymptotics are ramp-independent and depend only on the intrinsic spectrum
of the system. However, the intrinsic behavior is unobservable if the ramp is
not smooth enough. This is relevant for ramps to small interaction in the
fermionic Hubbard model, where the intrinsic cubic fall-off of the excitation
energy cannot be observed for a linear ramp due to its kinks at the beginning
and the end.Comment: 24 pages, 6 figure
Identifying Non-Resonant Kepler Planetary Systems
The Kepler mission has discovered a plethora of multiple transiting planet
candidate exosystems, many of which feature putative pairs of planets near mean
motion resonance commensurabilities. Identifying potentially resonant systems
could help guide future observations and enhance our understanding of planetary
formation scenarios. We develop and apply an algebraic method to determine
which Kepler 2-planet systems cannot be in a 1st-4th order resonance, given the
current, publicly available data. This method identifies when any potentially
resonant angle of a system must circulate. We identify and list 70
near-resonant systems which cannot actually reside in resonance, assuming a
widely-used formulation for deriving planetary masses from their observed radii
and that these systems do not contain unseen bodies that affect the
interactions of the observed planets. This work strengthens the argument that a
high fraction of exoplanetary systems may be near resonance but not actually in
resonance.Comment: 6 pages, 2 figures, 1 table, accepted for publication in MNRAS
Letter
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