1,539 research outputs found
Monopoles and the Emergence of Black Hole Entropy
One of the remarkable features of black holes is that they possess a
thermodynamic description, even though they do not appear to be statistical
systems. We use self-gravitating magnetic monopole solutions as tools for
understanding the emergence of this description as one goes from an ordinary
spacetime to one containing a black hole. We describe how causally distinct
regions emerge as a monopole solution develops a horizon. We define an entropy
that is naturally associated with these regions and that has a clear connection
with the Hawking-Bekenstein entropy in the critical black hole limit.Comment: 6 pages, one figure RevTe
Structure and stability of helices in square-well homopolymers
Recently, it has been demonstrated [Magee et al., Phys. Rev. Lett. 96, 207802
(2006)] that isolated, square-well homopolymers can spontaneously break chiral
symmetry and freeze into helical structures at sufficiently low temperatures.
This behavior is interesting because the square-well homopolymer is itself
achiral. In this work, we use event-driven molecular dynamics, combined with an
optimized parallel tempering scheme, to study this polymer model over a wide
range of parameters. We examine the conditions where the helix structure is
stable and determine how the interaction parameters of the polymer govern the
details of the helix structure. The width of the square well (proportional to
lambda) is found to control the radius of the helix, which decreases with
increasing well width until the polymer forms a coiled sphere for sufficiently
large wells. The helices are found to be stable for only a window of molecular
weights. If the polymer is too short, the helix will not form. If the polymer
is too long, the helix is no longer the minimum energy structure, and other
folded structures will form. The size of this window is governed by the chain
stiffness, which in this model is a function of the ratio of the monomer size
to the bond length. Outside this window, the polymer still freezes into a
locked structure at low temperature, however, unless the chain is sufficiently
stiff, this structure will not be unique and is similar to a glassy state.Comment: Submitted to Physical Review
How the orbital period of a test particle is modified by the Dvali-Gabadadze-Porrati gravity?
In addition to the pericentre \omega, the mean anomaly M and, thus, the mean
longitude \lambda, also the orbital period Pb and the mean motion of a test
particle are modified by the Dvali-Gabadadze-Porrati gravity. While the
correction to Pb depends on the mass of the central body and on the geometrical
features of the orbital motion around it, the correction to is independent
of them, up to terms of second order in the eccentricity . The latter one
amounts to about 2\times 10^-3 arcseconds per century. The present-day accuracy
in determining the mean motions of the inner planets of the Solar System from
radar ranging and differential Very Long Baseline Interferometry is
10^-2-5\times 10^-3 arcseconds per century, but it should be improved in the
near future when the data from the spacecraft to Mercury and Venus will be
available.Comment: LaTex, 7 pages, 13 references, no tables, no figures. Section 2.3
added. To appear in JCA
Helical structures from an isotropic homopolymer model
We present Monte Carlo simulation results for square-well homopolymers at a
series of bond lengths. Although the model contains only isotropic pairwise
interactions, under appropriate conditions this system shows spontaneous chiral
symmetry breaking, where the chain exists in either a left- or a right-handed
helical structure. We investigate how this behavior depends upon the ratio
between bond length and monomer radius.Comment: 10 pages, 3 figures, accepted for publication by Physical Review
Letter
Can black holes have Euclidean cores?
The search for regular black hole solutions in classical gravity leads us to
consider a core of Euclidean signature in the interior of a black hole.
Solutions of Lorentzian and Euclidean general relativity match in such a way
that energy densities and pressures of an isotropic perfect fluid form are
everywhere finite and continuous. Although the weak energy condition cannot be
satisfied for these solutions in general relativity, it can be when higher
derivative terms are added. A numerical study shows how the transition becomes
smoother in theories with more derivatives. As an alternative to the Euclidean
core, we also discuss a closely related time dependent orbifold construction
with a smooth space-like boundary inside the horizon.Comment: 14 pages with figures, version to appear in PR
Gravitational Properties of Monopole Spacetimes Near the Black Hole Threshold
Although nonsingular spacetimes and those containing black holes are
qualitatively quite different, there are continuous families of configurations
that connect the two. In this paper we use self-gravitating monopole solutions
as tools for investigating the transition between these two types of
spacetimes. We show how causally distinct regions emerge as the black hole
limit is achieved, even though the measurements made by an external observer
vary continuously. We find that near-critical solutions have a naturally
defined entropy, despite the absence of a true horizon, and that this has a
clear connection with the Hawking-Bekenstein entropy. We find that certain
classes of near-critical solutions display naked black hole behavior, although
they are not truly black holes at all. Finally, we present a numerical
simulation illustrating how an incident pulse of matter can induce the
dynamical collapse of a monopole into an extremal black hole. We discuss the
implications of this process for the third law of black hole thermodynamics.Comment: 23 pages, 4 figures RevTe
Quantum Melting of the Charge Density Wave State in 1T-TiSe2
We report a Raman scattering study of low-temperature, pressure-induced
melting of the CDW phase of 1T-TiSe2. Our Raman scattering measurements reveal
that the collapse of the CDW state occurs in three stages: (i) For P<5 kbar,
the pressure dependence of the CDW amplitude mode energies and intensities are
indicative of a ``crystalline'' CDW regime; (ii) for 5 < P < 25 kbar, there is
a decrease in the CDW amplitude mode energies and intensities with increasing
pressure that suggests a regime in which the CDW softens, and may decouple from
the lattice; and (iii) for P>25 kbar, the absence of amplitude modes reveals a
melted CDW regime.Comment: 5 pages, 4 figure
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