Model: lufercho/ArxvBert-ST_v2
Author: lufercho
Pipeline: sentence-similarity
Library: sentence-transformers
Tags: sentence-transformers, safetensors, bert, sentence-similarity, feature-extraction, generated_from_trainer, dataset_size:500, loss:MultipleNegativesRankingLoss, arxiv:1908.10084, arxiv:1705.00652, text-embeddings-inference, endpoints_compatible, region:us
Card metadata: tags: sentence-transformers, sentence-similarity, feature-extraction, generated_from_trainer, dataset_size:500, loss:MultipleNegativesRankingLoss
base_model: lufercho/ArxBert-MLM
widget: source_sentence: Entanglement increase from local interactions with
  not-completely-positive maps
sentences:   Simple examples are constructed that show the entanglement of two qubits
being both increased and decreased by interactions on just one of them. One of
the two qubits interacts with a third qubit, a control, that is never entangled
or correlated with either of the two entangled qubits and is never entangled,
but becomes correlated, with the system of those two qubits. The two entangled
qubits do not interact, but their state can change from maximally entangled to
separable or from separable to maximally entangled. Similar changes for the two
qubits are made with a swap operation between one of the qubits and a control;
then there are compensating changes of entanglement that involve the control.
When the entanglement increases, the map that describes the change of the state
of the two entangled qubits is not completely positive. Combination of two
independent interactions that individually give exponential decay of the
entanglement can cause the entanglement to not decay exponentially but,
instead, go to zero at a finite time.
,   Many extra-solar planets discovered over the past decade are gas giants in
tight orbits around their host stars. Due to the difficulties of forming these
`hot Jupiters' in situ, they are generally assumed to have migrated to their
present orbits through interactions with their nascent discs. In this paper, we
present a systematic study of giant planet migration in power law discs. We
find that the planetary migration rate is proportional to the disc surface
density. This is inconsistent with the assumption that the migration rate is
simply the viscous drift speed of the disc. However, this result can be
obtained by balancing the angular momentum of the planet with the viscous
torque in the disc. We have verified that this result is not affected by
adjusting the resolution of the grid, the smoothing length used, or the time at
which the planet is released to migrate.
,   We investigate the evolution of binary fractions in star clusters using
N-body models of up to 100000 stars. Primordial binary frequencies in these
models range from 5% to 50%. Simulations are performed with the NBODY4 code and
include a full mass spectrum of stars, stellar evolution, binary evolution and
the tidal field of the Galaxy. We find that the overall binary fraction of a
cluster almost always remains close to the primordial value, except at late
times when a cluster is near dissolution. A critical exception occurs in the
central regions where we observe a marked increase in binary fraction with time
-- a simulation starting with 100000 stars and 5% binaries reached a core
binary frequency as high as 40% at the end of the core-collapse phase
(occurring at 16 Gyr with ~20000 stars remaining). Binaries are destroyed in
the core by a variety of processes as a cluster evolves, but the combination of
mass-segregation and creation of new binaries in exchange interactions produces
the observed increase in relative number. We also find that binaries are cycled
into and out of cluster cores in a manner that is analogous to convection in
stars. For models of 100000 stars we show that the evolution of the core-radius
up to the end of the initial phase of core-collapse is not affected by the
exact value of the primordial binary frequency (for frequencies of 10% or
less). We discuss the ramifications of our results for the likely primordial
binary content of globular clusters.
, source_sentence: Vortex proliferation in the Berezinskii-Kosterlitz-Thouless regime on a
  two-dimensional lattice of Bose-Einstein condensates
sentences:   While the members of the Type IIn category of supernovae are united by the
presence of strong multicomponent Balmer emission lines in their spectra, they
are quite heterogeneous with respect to other properties such as Balmer line
profiles, light curves, strength of radio emission, and intrinsic brightness.
We are now beginning to see variety among SNe IIn in their polarimetric
characteristics as well, some but not all of which may be due to inclination
angle effects. The increasing number of known "hybrid" SNe with IIn-like
emission lines suggests that circumstellar material may be more common around
all types of SNe than previously thought. Investigation of the correlations
between spectropolarimetric signatures and other IIn attributes will help us
address the question of classification of "interacting SNe" and the possibility
of distinguishing different groups within the diverse IIn subclass.
,   (Abridged) We compare recent results from X-ray, strong lensing, weak
lensing, and optical observations with numerical simulations of the merging
galaxy cluster 1E0657-56. X-ray observations reveal a bullet-like subcluster
with a prominent bow shock, while lensing results show that the positions of
the total mass peaks are consistent with the centroids of the collisionless
galaxies (and inconsistent with the X-ray brightness peaks). Previous studies,
based on older observational datasets, have placed upper limits on the
self-interaction cross-section of dark matter per unit mass, sigma/m, using
simplified analytic techniques. In this work, we take advantage of new,
higher-quality observational datasets by running N-body simulations of
1E0657-56 that include the effects of self-interacting dark matter, and
comparing the results with observations. Furthermore, the recent data allow for
a new independent method of constraining sigma/m, based on the non-observation
of an offset between the bullet subcluster mass peak and galaxy centroid. This
new method places an upper limit (68% confidence) of sigma/m < 1.25 cm^2/g. If
we make the assumption that the subcluster and the main cluster had equal
mass-to-light ratios prior to the merger, we derive our most stringent
constraint of sigma/m < 0.7 cm^2/g, which comes from the consistency of the
subcluster's observed mass-to-light ratio with the main cluster's, and with the
universal cluster value, ruling out the possibility of a large fraction of dark
matter particles being scattered away due to collisions. Our limit is a slight
improvement over the previous result from analytic estimates, and rules out
most of the 0.5 - 5cm^2/g range invoked to explain inconsistencies between the
standard collisionless cold dark matter model and observations.
,   We observe the proliferation of vortices in the
Berezinskii-Kosterlitz-Thouless regime on a two-dimensional array of
Josephson-coupled Bose-Einstein condensates. As long as the Josephson
(tunneling) energy J exceeds the thermal energy T, the array is vortex-free.
With decreasing J/T, vortices appear in the system in ever greater numbers. We
confirm thermal activation as the vortex formation mechanism and obtain
information on the size of bound vortex pairs as J/T is varied.
, source_sentence: Geometric Complexity Theory V: On deciding nonvanishing of a generalized
  Littlewood-Richardson coefficient
sentences:   I shall present three arguments for the proposition that intelligent life is
very rare in the universe. First, I shall summarize the consensus opinion of
the founders of the Modern Synthesis (Simpson, Dobzhanski, and Mayr) that the
evolution of intelligent life is exceedingly improbable. Second, I shall
develop the Fermi Paradox: if they existed they'd be here. Third, I shall show
that if intelligent life were too common, it would use up all available
resources and die out. But I shall show that the quantum mechanical principle
of unitarity (actually a form of teleology!) requires intelligent life to
survive to the end of time. Finally, I shall argue that, if the universe is
indeed accelerating, then survival to the end of time requires that intelligent
life, though rare, to have evolved several times in the visible universe. I
shall argue that the acceleration is a consequence of the excess of matter over
antimatter in the universe. I shall suggest experiments to test these claims.
,   This article has been withdrawn because it has been merged with the earlier
article GCT3 (arXiv: CS/0501076 [cs.CC]) in the series. The merged article is
now available as:
  Geometric Complexity Theory III: on deciding nonvanishing of a
Littlewood-Richardson Coefficient, Journal of Algebraic Combinatorics, vol. 36,
issue 1, 2012, pp. 103-110. (Authors: Ketan Mulmuley, Hari Narayanan and Milind
Sohoni)
  The new article in this GCT5 slot in the series is:
  Geometric Complexity Theory V: Equivalence between blackbox derandomization
of polynomial identity testing and derandomization of Noether's Normalization
Lemma, in the Proceedings of FOCS 2012 (abstract), arXiv:1209.5993 [cs.CC]
(full version) (Author: Ketan Mulmuley)
,   We use high-resolution near-infrared spectroscopy from Keck Observatory to
measure the stellar velocity dispersions of 19 super star clusters (SSCs) in
the nuclear starburst of M82. The clusters have ages on the order of 10 Myr,
which is many times longer than the crossing times implied by their velocity
dispersions and radii. We therefore apply the Virial Theorem to derive the
kinematic mass for 15 of the SSCs. The SSCs have masses of 2 x 10^5 to 4 x 10^6
solar masses, with a total population mass of 1.4 x 10^7 solar masses.
Comparison of the loci of the young M82 SSCs and old Milky Way globular
clusters in a plot of radius versus velocity dispersion suggests that the SSCs
are a population of potential globular clusters. We present the mass function
for the SSCs, and find a power law fit with an index of gamma = -1.91 +/- 0.06.
This result is nearly identical to the mass function of young SSCs in the
Antennae galaxies.
, source_sentence: Teleparallel Version of the Stationary Axisymmetric Solutions and their
  Energy Contents
sentences:   We present a review of the discrete dipole approximation (DDA), which is a
general method to simulate light scattering by arbitrarily shaped particles. We
put the method in historical context and discuss recent developments, taking
the viewpoint of a general framework based on the integral equations for the
electric field. We review both the theory of the DDA and its numerical aspects,
the latter being of critical importance for any practical application of the
method. Finally, the position of the DDA among other methods of light
scattering simulation is shown and possible future developments are discussed.
,   This work contains the teleparallel version of the stationary axisymmetric
solutions. We obtain the tetrad and the torsion fields representing these
solutions. The tensor, vector and axial-vector parts of the torsion tensor are
evaluated. It is found that the axial-vector has component only along $\rho$
and $z$ directions. The three possibilities of the axial vector depending on
the metric function $B$ are discussed. The vector related with spin has also
been evaluated and the corresponding extra Hamiltonian is furnished. Further,
we use the teleparallel version of M$\ddot{o}$ller prescription to find the
energy-momentum distribution of the solutions. It is interesting to note that
(for $\lambda=1$) energy and momentum densities in teleparallel theory are
equal to the corresponding quantities in GR plus an additional quantity in
each, which may become equal under certain conditions. Finally, we discuss the
two special cases of the stationary axisymmetric solutions.
,   Most recently, both BaBar and Belle experiments found evidences of neutral
$D$ mixing. In this paper, we discuss the constraints on the strong phase
difference in $D^0 \to K\pi$ decay from the measurements of the mixing
parameters, $y^\prime$, $y_{CP}$ and $x$ at the $B$ factories. The sensitivity
of the measurement of the mixing parameter $y$ is estimated in BES-III
experiment at $\psi(3770)$ peak. We also make an estimate on the measurements
of the mixing rate $R_M$. Finally, the sensitivity of the strong phase
difference at BES-III are obtained by using data near the $D\bar{D}$ threshold
with CP tag technique at BES-III experiment.
, source_sentence: Approximation of the distribution of a stationary Markov process with
  application to option pricing
sentences:   We build a sequence of empirical measures on the space D(R_+,R^d) of
R^d-valued c\`adl\`ag functions on R_+ in order to approximate the law of a
stationary R^d-valued Markov and Feller process (X_t). We obtain some general
results of convergence of this sequence. Then, we apply them to Brownian
diffusions and solutions to L\'evy driven SDE's under some Lyapunov-type
stability assumptions. As a numerical application of this work, we show that
this procedure gives an efficient way of option pricing in stochastic
volatility models.
,   We provide a new estimate of the local supermassive black hole mass function
using (i) the empirical relation between supermassive black hole mass and the
Sersic index of the host spheroidal stellar system and (ii) the measured
(spheroid) Sersic indices drawn from 10k galaxies in the Millennium Galaxy
Catalogue. The observational simplicity of our approach, and the direct
measurements of the black hole predictor quantity, i.e. the Sersic index, for
both elliptical galaxies and the bulges of disc galaxies makes it
straightforward to estimate accurate black hole masses in early- and late-type
galaxies alike. We have parameterised the supermassive black hole mass function
with a Schechter function and find, at the low-mass end, a logarithmic slope
(1+alpha) of ~0.7 for the full galaxy sample and ~1.0 for the early-type galaxy
sample. Considering spheroidal stellar systems brighter than M_B = -18 mag, and
integrating down to black hole masses of 10^6 M_sun, we find that the local
mass density of supermassive black holes in early-type galaxies rho_{bh,
early-type} = (3.5+/-1.2) x 10^5 h^3_{70} M_sun Mpc^{-3}, and in late-type
galaxies rho_{bh, late-type} = (1.0+/-0.5) x 10^5 h^3_{70} M_sun Mpc^{-3}. The
uncertainties are derived from Monte Carlo simulations which include
uncertainties in the M_bh-n relation, the catalogue of Sersic indices, the
galaxy weights and Malmquist bias. The combined, cosmological, supermassive
black hole mass density is thus Omega_{bh, total} = (3.2+/-1.2) x 10^{-6} h_70.
That is, using a new and independent method, we conclude that (0.007+/-0.003)
h^3_{70} per cent of the universe's baryons are presently locked up in
supermassive black holes at the centres of galaxies.
,   We treat Koll\'ar's injectivity theorem from the analytic (or differential
geometric) viewpoint. More precisely, we give a curvature condition which
implies Koll\'ar type cohomology injectivity theorems. Our main theorem is
formulated for a compact K\"ahler manifold, but the proof uses the space of
harmonic forms on a Zariski open set with a suitable complete K\"ahler metric.
We need neither covering tricks, desingularizations, nor Leray's spectral
sequence.

pipeline_tag: sentence-similarity
library_name: sentence-transformers
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Created: 2024-11-25 14:19:17