59 research outputs found
Estimating Quasi-long-range Order via Renyi Entropies
We show how entanglement entropies allow for the estimation of
quasi-long-range order in one dimensional systems whose low-energy physics is
well captured by the Tomonaga-Luttinger liquid universality class. First, we
check our procedure in the exactly solvable XXZ spin-1/2 chain in its entire
critical region, finding very good agreement with Bethe ansatz results. Then,
we show how phase transitions between different dominant orders may be
efficiently estimated by considering the superfluid-charge density wave
transition in a system of dipolar bosons. Finally, we discuss the application
of this method to multispecies systems such as the one dimensional Hubbard
model. Our work represent the first proof of a direct relationship between the
Luttinger parameter and R\'enyi entropies in both bosonics and fermionic
lattice models.Comment: v2: minimal changes, 6 pages, 7 figures, accepted for publication in
Phys. Rev.
Local and nonlocal pressure Hessian effects in real and synthetic fluid turbulence
The Lagrangian dynamics of the velocity gradient tensor A in isotropic and
homogeneous turbulence depend on the joint action of the self-streching term
and the pressure Hessian. Existing closures for pressure effects in terms of A
are unable to reproduce one important statistical role played by the
anisotropic part of the pressure Hessian, namely the redistribution of the
probabilities towards enstrophy production dominated regions. As a step towards
elucidating the required properties of closures, we study several synthetic
velocity fields and how well they reproduce anisotropic pressure effects. It is
found that synthetic (i) Gaussian, (ii) Multifractal and (iii) Minimal Turnover
Lagrangian Map (MTLM) incompressible velocity fields reproduce many features of
real pressure fields that are obtained from numerical simulations of the Navier
Stokes equations, including the redistribution towards enstrophy-production
regions. The synthetic fields include both spatially local, and nonlocal,
anisotropic pressure effects. However, we show that the local effects appear to
be the most important ones: by assuming that the pressure Hessian is local in
space, an expression in terms of the Hessian of the second invariant Q of the
velocity gradient tensor can be obtained. This term is found to be well
correlated with the true pressure Hessian both in terms of eigenvalue
magnitudes and eigenvector alignments.Comment: 10 pages, 4 figures, minor changes, final version, published in Phys.
Fluid
Critical properties and R\'enyi entropies of the spin-3/2 XXZ chain
We discuss entanglement and critical properties of the spin-3/2 XXZ chain in
its entire gapless region. Employing density-matrix renormalization group
calculations combined with different methods based on level spectroscopy,
correlation functions and entanglement entropies, we determine the sound
velocity and the Luttinger parameter of the model as a function of the
anisotropy parameter. Then, we focus on entanglement properties by
systematically studying the behavior of R\'enyi entropies under both open and
periodic boundary conditions, providing further evidence of recent findings
about entanglement entropies of excited states in conformal field theory.Comment: 8 pages, 10 figures; small text revisions and a new figure. Accepted
for publication in Phys. Rev.
Polarimetry of the superluminous supernova LSQ14mo: no evidence for significant deviations from spherical symmetry
We present the first polarimetric observations of a Type I superluminous
supernova (SLSN). LSQ14mo was observed with VLT/FORS2 at five different epochs
in the V band, with the observations starting before maximum light and spanning
26 days in the rest frame (z=0.256). During this period, we do not detect any
statistically significant evolution (< 2) in the Stokes parameters. The
average values we obtain, corrected for interstellar polarisation in the
Galaxy, are Q = -0.01% ( 0.15%) and U = - 0.50% ( 0.14%). This low
polarisation can be entirely due to interstellar polarisation in the SN host
galaxy. We conclude that, at least during the period of observations and at the
optical depths probed, the photosphere of LSQ14mo does not present significant
asymmetries, unlike most lower-luminosity hydrogen-poor SNe Ib/c.
Alternatively, it is possible that we may have observed LSQ14mo from a special
viewing angle. Supporting spectroscopy and photometry confirm that LSQ14mo is a
typical SLSN I. Further studies of the polarisation of Type I SLSNe are
required to determine whether the low levels of polarisation are a
characteristic of the entire class and to also study the implications for the
proposed explosion models.Comment: ApJ Letters, 4 Figures, 3 Tables. The previous version was accepted.
This version contains minor modifications to match proofs (as much as
possible
The Carnegie Supernova Project I : Analysis of stripped-envelope supernova light curves
Stripped-envelope (SE) supernovae (SNe) include H-poor (Type IIb), H-free (Type Ib), and He-free (Type Ic) events thought to be associated with the deaths of massive stars. The exact nature of their progenitors is a matter of debate with several lines of evidence pointing towards intermediate mass (Minit15(B), while the post maximum light curves reveals a correlation between the late-time linear slope and Δm15. Making use of the full set of optical and near-IR photometry, combined with robust host-galaxy extinction corrections, comprehensive bolometric light curves are constructed and compared to both analytic and hydrodynamical models. This analysis finds consistent results among the two different modeling techniques and from the hydrodynamical models we obtained ejecta masses of 1.1–6.2M⊙, 56Ni masses of 0.03–0.35M⊙, and explosion energies (excluding two SNe Ic-BL) of 0.25–3.0 × 1051 erg. Our analysis indicates that adopting κ = 0.07 cm2 g-1 as the mean opacity serves to be a suitable assumption when comparing Arnett-model results to those obtained from hydrodynamical calculations. We also find that adopting He I and O I line velocities to infer the expansion velocity in He-rich and He-poor SNe, respectively, provides ejecta masses relatively similar to those obtained by using the Fe II line velocities, although the use of Fe II as a diagnostic does imply higher explosion energies. The inferred range of ejecta masses are compatible with intermediate mass (MZAMS ≤ 20M⊙) progenitor stars in binary systems for the majority of SE SNe. Furthermore, our hydrodynamical modeling of the bolometric light curves suggests a significant fraction of the sample may have experienced significant mixing of 56Ni, particularly in the case of SNe Ic.Facultad de Ciencias Astronómicas y GeofÃsica
The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission
We present imaging and spectroscopy of a hydrogen-poor superluminous supernova (SLSN) discovered by the intermediate Palomar Transient Factory, iPTF 13ajg. At a redshift of z = 0.7403, derived from narrow absorption lines, iPTF 13ajg peaked at an absolute magnitude of M u, AB = -22.5, one of the most luminous supernovae to date. The observed bolometric peak luminosity of iPTF 13ajg is 3.2 × 1044 erg s-1, while the estimated total radiated energy is 1.3 × 1051 erg. We detect narrow absorption lines of Mg I, Mg II, and Fe II, associated with the cold interstellar medium in the host galaxy, at two different epochs with X-shooter at the Very Large Telescope. From Voigt profile fitting, we derive the column densities log N(Mg I) =11.94 ± 0.06, log N(Mg II) =14.7 ± 0.3, and log N(Fe II) =14.25 ± 0.10. These column densities, as well as the Mg I and Mg II equivalent widths of a sample of hydrogen-poor SLSNe taken from the literature, are at the low end of those derived for gamma-ray bursts (GRBs) whose progenitors are also thought to be massive stars. This suggests that the environments of hydrogen-poor SLSNe and GRBs are different. From the nondetection of Fe II fine-structure absorption lines, we derive a lower limit on the distance between the supernova and the narrow-line absorbing gas of 50 pc. The neutral gas responsible for the absorption in iPTF 13ajg exhibits a single narrow component with a low velocity width, ΔV = 76 km s-1, indicating a low-mass host galaxy. No host galaxy emission lines are detected, leading to an upper limit on the unobscured star formation rate (SFR) of SFR. Late-time imaging shows the iPTF 13ajg host galaxy to be faint, with g AB 27.0 and R AB ≥ 26.0 mag, corresponding to M B, Vega ≳ -17.7 mag. © 2014. The American Astronomical Society. All rights reserved.
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