1,575 research outputs found
Systematic characterization of thermodynamic and dynamical phase behavior in systems with short-ranged attraction
In this paper we demonstrate the feasibility and utility of an augmented
version of the Gibbs ensemble Monte Carlo method for computing the phase
behavior of systems with strong, extremely short-ranged attractions. For
generic potential shapes, this approach allows for the investigation of
narrower attractive widths than those previously reported. Direct comparison to
previous self-consistent Ornstein-Zernike approximation calculations are made.
A preliminary investigation of out-of-equilibrium behavior is also performed.
Our results suggest that the recent observations of stable cluster phases in
systems without long-ranged repulsions are intimately related to gas-crystal
and metastable gas-liquid phase separation.Comment: 10 pages, 8 figure
Phase Transformations in Binary Colloidal Monolayers
Phase transformations can be difficult to characterize at the microscopic
level due to the inability to directly observe individual atomic motions. Model
colloidal systems, by contrast, permit the direct observation of individual
particle dynamics and of collective rearrangements, which allows for real-space
characterization of phase transitions. Here, we study a quasi-two-dimensional,
binary colloidal alloy that exhibits liquid-solid and solid-solid phase
transitions, focusing on the kinetics of a diffusionless transformation between
two crystal phases. Experiments are conducted on a monolayer of magnetic and
nonmagnetic spheres suspended in a thin layer of ferrofluid and exposed to a
tunable magnetic field. A theoretical model of hard spheres with point dipoles
at their centers is used to guide the choice of experimental parameters and
characterize the underlying materials physics. When the applied field is normal
to the fluid layer, a checkerboard crystal forms; when the angle between the
field and the normal is sufficiently large, a striped crystal assembles. As the
field is slowly tilted away from the normal, we find that the transformation
pathway between the two phases depends strongly on crystal orientation, field
strength, and degree of confinement of the monolayer. In some cases, the
pathway occurs by smooth magnetostrictive shear, while in others it involves
the sudden formation of martensitic plates.Comment: 13 pages, 7 figures. Soft Matter Latex template was used. Published
online in Soft Matter, 201
The Spitzer search for the transits of HARPS low-mass planets - I. No transit for the super-Earth HD 40307b
We have used Spitzer and its IRAC camera to search for the transit of the
super-Earth HD 40307b. The transiting nature of the planet could not be firmly
discarded from our first photometric monitoring of a transit window because of
the uncertainty coming from the modeling of the photometric baseline. To obtain
a firm result, two more transit windows were observed and a global Bayesian
analysis of the three IRAC time series and the HARPS radial velocities was
performed. Unfortunately, any transit of the planet during the observed phase
window is firmly discarded, while the probability that the planet transits but
that the eclipse was missed by our observations is nearly negligible (0.26%).Comment: Submitted to A&
Hard sphere crystallization gets rarer with increasing dimension
We recently found that crystallization of monodisperse hard spheres from the
bulk fluid faces a much higher free energy barrier in four than in three
dimensions at equivalent supersaturation, due to the increased geometrical
frustration between the simplex-based fluid order and the crystal [J.A. van
Meel, D. Frenkel, and P. Charbonneau, Phys. Rev. E 79, 030201(R) (2009)]. Here,
we analyze the microscopic contributions to the fluid-crystal interfacial free
energy to understand how the barrier to crystallization changes with dimension.
We find the barrier to grow with dimension and we identify the role of
polydispersity in preventing crystal formation. The increased fluid stability
allows us to study the jamming behavior in four, five, and six dimensions and
compare our observations with two recent theories [C. Song, P. Wang, and H. A.
Makse, Nature 453, 629 (2008); G. Parisi and F. Zamponi, Rev. Mod. Phys, in
press (2009)].Comment: 15 pages, 5 figure
New data and the hard pomeron
New structure-function data are in excellent agreement with the existence of
a hard pomeron, with intercept about 1.4. It gives a very economical
description of the data. Having fixed 2 parameters from the data for the
real-photon cross section , we need just 5 further
parameters to fit the data for with . The available
data range from to 35 GeV. With guesses consistent with
dimensional counting for the dependences of our three separate terms, the
fit extends well to larger and to GeV. With no additional
parameters, it gives a good description of data for the charm structure
function from to 130 GeV. The two pomerons also give
a good description of both the and the dependence of .Comment: 11 pages, plain tex, with 10 figures embedded using epsf. (Spurious
figure removed.
The 8 Micron Phase Variation of the Hot Saturn HD 149026b
We monitor the star HD 149026 and its Saturn-mass planet at 8.0 micron over
slightly more than half an orbit using the Infrared Array Camera (IRAC) on the
Spitzer Space Telescope. We find an increase of 0.0227% +/- 0.0066% (3.4 sigma
significance) in the combined planet-star flux during this interval. The
minimum flux from the planet is 45% +/- 19% of the maximum planet flux,
corresponding to a difference in brightness temperature of 480 +/- 140 K
between the two hemispheres. We derive a new secondary eclipse depth of 0.0411%
+/- 0.0076% in this band, corresponding to a dayside brightness temperature of
1440 +/- 150 K. Our new secondary eclipse depth is half that of a previous
measurement (3.0 sigma difference) in this same bandpass by Harrington et al.
(2007). We re-fit the Harrington et al. (2007) data and obtain a comparably
good fit with a smaller eclipse depth that is consistent with our new value. In
contrast to earlier claims, our new eclipse depth suggests that this planet's
dayside emission spectrum is relatively cool, with an 8 micron brightness
temperature that is less than the maximum planet-wide equilibrium temperature.
We measure the interval between the transit and secondary eclipse and find that
that the secondary eclipse occurs 20.9 +7.2 / -6.5 minutes earlier (2.9 sigma)
than predicted for a circular orbit, a marginally significant result. This
corresponds to e*cos(omega) = -0.0079 +0.0027 / -0.0025 where e is the planet's
orbital eccentricity and omega is the argument of pericenter.Comment: 17 pages, 12 figure, accepted for publication in Ap
Inverting Phase Functions to Map Exoplanets
We describe how to generate a longitudinal brightness map for a tidally
locked exoplanet from its phase function light curve. We operate under a number
of simplifying assumptions, neglecting limb darkening/brightening, star spots,
detector ramps, as well as time-variability over a single planetary rotation.
We develop the transformation from a planetary brightness map to a phase
function light curve and simplify the expression for the case of an edge-on
system. We introduce two models--composed of longitudinal slices of uniform
brightness, and sinusoidally varying maps, respectively--which greatly simplify
the transformation from map to light curve. We discuss numerical approaches to
extracting a longitudinal map from a phase function light curve, explaining how
to estimate the uncertainty in a computed map and how to choose an appropriate
number of fit parameters. We demonstrate these techniques on a simulated map
and discuss the uses and limitations of longitudinal maps. The sinusoidal model
provides a better fit to the planet's underlying brightness map, although the
slice model is more appropriate for light curves which only span a fraction of
the planet's orbit. Regardless of which model is used, we find that there is a
maximum of ~5 free parameters which can be meaningfully fit based on a full
phase function light curve, due to the insensitivity of the latter to certain
modes of the map.Comment: 5 pages, 3 figures, accepted for publication in ApJ
Multiepoch Radial Velocity Observations of L Dwarfs
We report on the development of a technique for precise radial-velocity
measurements of cool stars and brown dwarfs in the near infrared. Our technique
is analogous to the Iodine (I2) absorption cell method that has proven so
successful in the optical regime. We rely on telluric CH4 absorption features
to serve as a wavelength reference, relative to which we measure Doppler shifts
of the CO and H2O features in the spectra of our targets. We apply this
technique to high-resolution (R~50,000) spectra near 2.3 micron of nine L
dwarfs taken with the Phoenix instrument on Gemini-South and demonstrate a
typical precision of 300 m/s. We conduct simulations to estimate our expected
precision and show our performance is currently limited by the signal-to-noise
of our data. We present estimates of the rotational velocities and systemic
velocities of our targets. With our current data, we are sensitive to
companions with M sin i > 2MJ in orbits with periods less than three days. We
identify no companions in our current data set. Future observations with
improved signal-to-noise should result in radial-velocity precision of 100 m/s
for L dwarfs.Comment: Accepted for publication in ApJ, 24 pages, 7 figure
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