12,285 research outputs found
Scattering functions of knotted ring polymers
We discuss the scattering function of a Gaussian random polygon with N nodes
under a given topological constraint through simulation. We obtain the Kratky
plot of a Gaussian polygon of N=200 having a fixed knot for some different
knots such as the trivial, trefoil and figure-eight knots. We find that some
characteristic properties of the different Kratky plots are consistent with the
distinct values of the mean square radius of gyration for Gaussian polygons
with the different knots.Comment: 4pages, 3figures, 3table
Ram pressure stripping and galaxy orbits: The case of the Virgo cluster
We investigate the role of ram pressure stripping in the Virgo cluster using
N-body simulations. Radial orbits within the Virgo cluster's gravitational
potential are modeled and analyzed with respect to ram pressure stripping. The
N-body model consists of 10000 gas cloud complexes which can have inelastic
collisions. Ram pressure is modeled as an additional acceleration on the clouds
located at the surface of the gas distribution in the direction of the galaxy's
motion within the cluster. We made several simulations changing the orbital
parameters in order to recover different stripping scenarios using realistic
temporal ram pressure profiles. We investigate systematically the influence of
the inclination angle between the disk and the orbital plane of the galaxy on
the gas dynamics. We show that ram pressure can lead to a temporary increase of
the central gas surface density. In some cases a considerable part of the total
atomic gas mass (several 10^8 M_solar) can fall back onto the galactic disk
after the stripping event. A quantitative relation between the orbit parameters
and the resulting HI deficiency is derived containing explicitly the
inclination angle between the disk and the orbital plane. The comparison
between existing HI observations and the results of our simulations shows that
the HI deficiency depends strongly on galaxy orbits. It is concluded that the
scenario where ram pressure stripping is responsible for the observed HI
deficiency is consistent with all HI 21cm observations in the Virgo cluster.Comment: 29 pages with 21 figures. Accepted for publication in Ap
Does the Fornax dwarf spheroidal have a central cusp or core?
The dark matter dominated Fornax dwarf spheroidal has five globular clusters
orbiting at ~1 kpc from its centre. In a cuspy CDM halo the globulars would
sink to the centre from their current positions within a few Gyrs, presenting a
puzzle as to why they survive undigested at the present epoch. We show that a
solution to this timing problem is to adopt a cored dark matter halo. We use
numerical simulations and analytic calculations to show that, under these
conditions, the sinking time becomes many Hubble times; the globulars
effectively stall at the dark matter core radius. We conclude that the Fornax
dwarf spheroidal has a shallow inner density profile with a core radius
constrained by the observed positions of its globular clusters. If the phase
space density of the core is primordial then it implies a warm dark matter
particle and gives an upper limit to its mass of ~0.5 keV, consistent with that
required to significantly alleviate the substructure problem.Comment: 6 pages, 5 figures, accepted for publication in MNRAS, high
resolution simulations include
Velocity Structure of Self-Similar Spherically Collapsed Halos
Using a generalized self-similar secondary infall model, which accounts for
tidal torques acting on the halo, we analyze the velocity profiles of halos in
order to gain intuition for N-body simulation results. We analytically
calculate the asymptotic behavior of the internal radial and tangential kinetic
energy profiles in different radial regimes. We then numerically compute the
velocity anisotropy and pseudo-phase-space density profiles and compare them to
recent N-body simulations. For cosmological initial conditions, we find both
numerically and analytically that the anisotropy profile asymptotes at small
radii to a constant set by model parameters. It rises on intermediate scales as
the velocity dispersion becomes more radially dominated and then drops off at
radii larger than the virial radius where the radial velocity dispersion
vanishes in our model. The pseudo-phase-space density is universal on
intermediate and large scales. However, its asymptotic slope on small scales
depends on the halo mass and on how mass shells are torqued after turnaround.
The results largely confirm N-body simulations but show some differences that
are likely due to our assumption of a one-dimensional phase space manifold.Comment: 11 pages, 4 figures. Accepted by PR
GHASP : an H alpha kinematic survey of spiral and irregular galaxies. V. Dark matter distribution in 36 nearby spiral galaxies
The results obtained from a study of the mass distribution of 36 spiral
galaxies are presented. The galaxies were observed using Fabry-Perot
interferometry as part of the GHASP survey. The main aim of obtaining high
resolution H alpha 2D velocity fields is to define more accurately the rising
part of the rotation curves which should allow to better constrain the
parameters of the mass distribution. The H alpha velocities were combined with
low resolution HI data from the literature, when available. Combining the
kinematical data with photometric data, mass models were derived from these
rotation curves using two different functional forms for the halo: an
isothermal sphere and an NFW profile. For the galaxies already modeled by other
authors, the results tend to agree. Our results point at the existence of a
constant density core in the center of the dark matter halos rather than a
cuspy core, whatever the type of the galaxy from Sab to Im. This extends to all
types the result already obtained by other authors studying dwarf and LSB
galaxies but would necessitate a larger sample of galaxies to conclude more
strongly. Whatever model is used (ISO or NFW), small core radius halos have
higher central densities, again for all morphological types. We confirm
different halo scaling laws, such as the correlations between the core radius
and the central density of the halo with the absolute magnitude of a galaxy:
low luminosity galaxies have small core radius and high central density. We
find that the product of the central density with the core radius of the dark
matter halo is nearly constant, whatever the model and whatever the absolute
magnitude of the galaxy. This suggests that the halo surface density is
independent from the galaxy type.Comment: 21 pages, 14 figures. MNRAS (accepted october 3rd 2007
Greedy Forwarding in Dynamic Scale-Free Networks Embedded in Hyperbolic Metric Spaces
We show that complex (scale-free) network topologies naturally emerge from
hyperbolic metric spaces. Hyperbolic geometry facilitates maximally efficient
greedy forwarding in these networks. Greedy forwarding is topology-oblivious.
Nevertheless, greedy packets find their destinations with 100% probability
following almost optimal shortest paths. This remarkable efficiency sustains
even in highly dynamic networks. Our findings suggest that forwarding
information through complex networks, such as the Internet, is possible without
the overhead of existing routing protocols, and may also find practical
applications in overlay networks for tasks such as application-level routing,
information sharing, and data distribution
Excitons in type-II quantum dots: Finite offsets
Quantum size effects for an exciton attached to a spherical quantum dot are
calculated by a variational approach. The band line-ups are assumed to be
type-II with finite offsets. The dependence of the exciton binding energy upon
the dot radius and the offsets is studied for different sets of electron and
hole effective masses
On the equilibrium morphology of systems drawn from spherical collapse experiments
We present a purely theoretical study of the morphological evolution of
self-gravitating systems formed through the dissipationless collapse of N-point
sources. We explore the effects of resolution in mass and length on the growth
of triaxial structures formed by an instability triggered by an excess of
radial orbits. We point out that as resolution increases, the equilibria shift,
from mildly prolate, to oblate. A number of particles N ~= 100000 or larger is
required for convergence of axial aspect ratios. An upper bound for the
softening, e ~ 1/256, is also identified. We then study the properties of a set
of equilibria formed from scale-free cold initial mass distributions, ro ~ r^-g
with 0 <= g <= 2. Oblateness is enhanced for initially more peaked structures
(larger values of g). We map the run of density in space and find no evidence
for a power-law inner structure when g <= 3/2 down to a mass fraction <~0.1 per
cent of the total. However, when 3/2 < g <= 2, the mass profile in equilibrium
is well matched by a power law of index ~g out to a mass fraction ~ 10 per
cent. We interpret this in terms of less-effective violent relaxation for more
peaked profiles when more phase mixing takes place at the centre. We map out
the velocity field of the equilibria and note that at small radii the velocity
coarse-grained distribution function (DF) is Maxwellian to a very good
approximation.Comment: 16 page
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