7,708 research outputs found
Numerical test of the Cardy-Jacobsen conjecture in the site-diluted Potts model in three dimensions
We present a microcanonical Monte Carlo simulation of the site-diluted Potts
model in three dimensions with eight internal states, partly carried out in the
citizen supercomputer Ibercivis. Upon dilution, the pure model's first-order
transition becomes of the second-order at a tricritical point. We compute
accurately the critical exponents at the tricritical point. As expected from
the Cardy-Jacobsen conjecture, they are compatible with their Random Field
Ising Model counterpart. The conclusion is further reinforced by comparison
with older data for the Potts model with four states.Comment: Final version. 9 pages, 9 figure
The out-equilibrium 2D Ising spin glass: almost, but not quite, a free-field theory
We consider the spatial correlation function of the two-dimensional Ising
spin glass under out-equilibrium conditions. We pay special attention to the
scaling limit reached upon approaching zero temperature. The field-theory of a
non-interacting field makes a surprisingly good job at describing the spatial
shape of the correlation function of the out-equilibrium Edwards-Anderson Ising
model in two dimensions.Comment: 20 pages + 5 Figure
Effect of Dilution on First Order Transitions: The Three Dimensional Three States Potts Model
We have studied numerically the effect of quenched site dilution on a first
order phase transition in three dimensions. We have simulated the site diluted
three states Potts model studying in detail the second order region of its
phase diagram. We have found that the exponent is compatible with the one
of the three dimensional diluted Ising model whereas the exponent is
definitely different.Comment: RevTex. 6 pages and 6 postscript figure
Constraining the evolution of stellar rotation using solar twins
The stellar Rotation Age relation is commonly considered as a useful
tool to derive reliable ages for Sun-like stars. However, in the light of
\kepler\ data, the presence of apparently old and fast rotators that do not
obey the usual gyrochronology relations led to the hypothesis of weakened
magnetic breaking in some stars. In this letter, we constrain the solar
rotation evolutionary track using solar twins. Predicted rotational periods as
a function of mass, age, [Fe/H] and given critical Rossby number () were estimated for the entire rotational sample. Our analysis favors
the smooth rotational evolution scenario and suggests that, if the magnetic
weakened breaking scenario takes place at all, it should arise after or ages 5.3 Gyr (at 95 confidence level).Comment: 5 pages, 3 figures, accepted for publication in MNRA
NGC 6309, a Planetary Nebula that Shifted from Round to Multipolar
We present new narrow-band Ha, [N II], and [O III] high-resolution images of
the quadrupolar planetary nebula (PN) NGC 6309 that show in great detail its
bipolar lobes and reveal new morphological features. New high- and
low-dispersion long-slit spectra have been obtained to help in the
investigation of the new nebular components. The images and spectra unveil two
diffuse blobs, one of them located at 55 arcsec from the central star along the
NE direction (PA= +71) and the other at 78 arcsec in the SW direction (PA=
-151). Therefore, these structures do not share the symmetry axes of the inner
bipolar outflows. Their radial velocities relative to the system are quite low:
+3 and -4 km/s, respectively. Spectroscopic data confirm a high [O III] to Ha
ratio, indicating that the blobs are being excited by the UV flux from the
central star. Our images convincingly show a spherical halo 60 arcsec in
diameter encircling the quadrupolar nebula. The expansion velocity of this
shell is low, 66 km/s. The software SHAPE has been used to construct a
morpho-kinematic model for the ring and the bipolar flows that implies an age
of 4,000 yrs, the expansion of the halo sets a lower limit for its age 46,000
yrs, and the very low expansion of the blobs suggests they are part of a large
structure corresponding to a mass ejection that took place 150,000 yrs ago. In
NGC 6309 we have direct evidence of a change in the geometry of mass-loss, from
spherical in the halo to axially-symmetric in the two pairs of bipolar lobes.Comment: 8 pages, 7 figures, Accepted for publication in MNRA
Comment on "Evidence of Non-Mean-Field-Like Low-Temperature Behavior in the Edwards-Anderson Spin-Glass Model"
A recent interesting paper [Yucesoy et al. Phys. Rev. Lett. 109, 177204
(2012), arXiv:1206:0783] compares the low-temperature phase of the 3D
Edwards-Anderson (EA) model to its mean-field counterpart, the
Sherrington-Kirkpatrick (SK) model. The authors study the overlap distributions
P_J(q) and conclude that the two models behave differently. Here we notice that
a similar analysis using state-of-the-art, larger data sets for the EA model
(generated with the Janus computer) leads to a very clear interpretation of the
results of Yucesoy et al., showing that the EA model behaves as predicted by
the replica symmetry breaking (RSB) theory.Comment: Version accepted for publication in PRL. 1 page, 1 figur
Solving the Boltzmann equation in N log N
In [C. Mouhot and L. Pareschi, "Fast algorithms for computing the Boltzmann
collision operator," Math. Comp., to appear; C. Mouhot and L. Pareschi, C. R.
Math. Acad. Sci. Paris, 339 (2004), pp. 71-76], fast deterministic algorithms
based on spectral methods were derived for the Boltzmann collision operator for
a class of interactions including the hard spheres model in dimension three.
These algorithms are implemented for the solution of the Boltzmann equation in
two and three dimension, first for homogeneous solutions, then for general non
homogeneous solutions. The results are compared to explicit solutions, when
available, and to Monte-Carlo methods. In particular, the computational cost
and accuracy are compared to those of Monte-Carlo methods as well as to those
of previous spectral methods. Finally, for inhomogeneous solutions, we take
advantage of the great computational efficiency of the method to show an
oscillation phenomenon of the entropy functional in the trend to equilibrium,
which was suggested in the work [L. Desvillettes and C. Villani, Invent. Math.,
159 (2005), pp. 245-316].Comment: 32 page
Microcanonical finite-size scaling in specific heat diverging 2nd order phase transitions
A Microcanonical Finite Site Ansatz in terms of quantities measurable in a
Finite Lattice allows to extend phenomenological renormalization (the so called
quotients method) to the microcanonical ensemble. The Ansatz is tested
numerically in two models where the canonical specific-heat diverges at
criticality, thus implying Fisher-renormalization of the critical exponents:
the 3D ferromagnetic Ising model and the 2D four-states Potts model (where
large logarithmic corrections are known to occur in the canonical ensemble). A
recently proposed microcanonical cluster method allows to simulate systems as
large as L=1024 (Potts) or L=128 (Ising). The quotients method provides
extremely accurate determinations of the anomalous dimension and of the
(Fisher-renormalized) thermal exponent. While in the Ising model the
numerical agreement with our theoretical expectations is impressive, in the
Potts case we need to carefully incorporate logarithmic corrections to the
microcanonical Ansatz in order to rationalize our data.Comment: 13 pages, 8 figure
gem-Dibromocyclopropanes and enzymatically derived cis-1,2-dihydrocatechols as building blocks in alkaloid synthesis
The application of the title building blocks, the 6,6-dibromobicyclo[3.1.0]hexanes
and the cis-1,2-dihydrocatechols, to the total synthesis of crinine and lycorinine alkaloids is
described.We thank the Australian Research Council and the Institute of Advanced Studies for generous financial
support
Spectroscopic binaries in the Solar Twin Planet Search program: from substellar-mass to M dwarf companions
Previous studies on the rotation of Sun-like stars revealed that the
rotational rates of young stars converge towards a well-defined evolution that
follows a power-law decay. It seems, however, that some binary stars do not
obey this relation, often by displaying enhanced rotational rates and activity.
In the Solar Twin Planet Search program we observed several solar twin
binaries, and found a multiplicity fraction of in the whole
sample; moreover, at least three of these binaries (HIP 19911, HIP 67620 and
HIP 103983) clearly exhibit the aforementioned anomalies. We investigated the
configuration of the binaries in the program, and discovered new companions for
HIP 6407, HIP 54582, HIP 62039 and HIP 30037, of which the latter is orbited by
a M brown dwarf in a 1-month long orbit. We report the orbital
parameters of the systems with well-sampled orbits and, in addition, the lower
limits of parameters for the companions that only display a curvature in their
radial velocities. For the linear trend binaries, we report an estimate of the
masses of their companions when their observed separation is available, and a
minimum mass otherwise. We conclude that solar twin binaries with low-mass
stellar companions at moderate orbital periods do not display signs of a
distinct rotational evolution when compared to single stars. We confirm that
the three peculiar stars are double-lined binaries, and that their companions
are polluting their spectra, which explains the observed anomalies.Comment: 13 pages, 7 figures, accepted for publication in MNRA
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