90 research outputs found
Leaf color and vine size are related to yield in a phylloxera-infested vineyard
The uneven spread of phylloxera infestation and associated vine symptoms in vineyards usually complicates yield estimates and vineyard replacement decisions. In a Cabernet Sauvignon vineyard with AXR#1 rootstock the current season's and following season's yields of 40 vine plots correlated (r ≥ 0.77, p ≤ 0.05) with early to midseason leaf and canopy spectra measured in the field, laboratory and remotely with aircraft-borne sensors
Phantom stars and topology change
In this work, we consider time-dependent dark energy star models, with an
evolving parameter crossing the phantom divide, . Once in
the phantom regime, the null energy condition is violated, which physically
implies that the negative radial pressure exceeds the energy density.
Therefore, an enormous negative pressure in the center may, in principle, imply
a topology change, consequently opening up a tunnel and converting the dark
energy star into a wormhole. The criteria for this topology change are
discussed, in particular, we consider the Morse Index analysis and a Casimir
energy approach involving quasi-local energy difference calculations that may
reflect or measure the occurrence of a topology change. We denote these exotic
geometries consisting of dark energy stars (in the phantom regime) and phantom
wormholes as phantom stars. The final product of this topological change,
namely, phantom wormholes, have far-reaching physical and cosmological
implications, as in addition to being used for interstellar shortcuts, an
absurdly advanced civilization may manipulate these geometries to induce closed
timelike curves, consequently violating causality.Comment: 19 pages, 13 figures. V2: Extended version of the paper accepted for
publication in Physical Review
Axially symmetric rotating traversable wormholes
This paper generalizes the static and spherically symmetric traversable
wormhole geometry to a rotating axially symmetric one with a time-dependent
angular velocity by means of an exact solution. It was found that the violation
of the weak energy condition, although unavoidable, is considerably less severe
than in the static spherically symmetric case. The radial tidal constraint is
more easily met due to the rotation. Similar improvements are seen in one of
the lateral tidal constraints. The magnitude of the angular velocity may have
little effect on the weak energy condition violation for an axially symmetric
wormhole. For a spherically symmetric one, however, the violation becomes less
severe with increasing angular velocity. The time rate of change of the angular
velocity, on the other hand, was found to have no effect at all. Finally, the
angular velocity must depend only on the radial coordinate, confirming an
earlier result.Comment: 17 pages, AMSTe
Magnetic strings in anti-de Sitter General Relativity
We obtain spacetimes generated by static and spinning magnetic string sources
in Einstein Relativity with negative cosmological constant. Since the spacetime
is asymptotically a cylindrical anti-de Sitter spacetime, we will be able to
calculate the mass, momentum, and electric charge of the solutions. We find two
families of solutions, one with longitudinal magnetic field and the other with
angular magnetic field. The source for the longitudinal magnetic field can be
interpreted as composed by a system of two symmetric and superposed
electrically charged lines with one of the electrically charged lines being at
rest and the other spinning. The angular magnetic field solution can be
similarly interpreted as composed by charged lines but now one is at rest and
the other has a velocity along the axis. This solution cannot be extended down
to the origin.Comment: Latex, 26 page
Gravastar Solutions with Continuous Pressures and Equation of State
We study the gravitational vacuum star (gravastar) configuration as proposed
by other authors in a model where the interior de Sitter spacetime segment is
continuously extended to the exterior Schwarzschild spacetime. The multilayered
structure in previous papers is replaced by a continuous stress-energy tensor
at the price of introducing anisotropy in the (fluid) model of the gravastar.
Either with an ansatz for the equation of state connecting the radial and
tangential pressure or with a calculated equation of state with
non-homogeneous energy/fluid density, solutions are obtained which in all
aspects satisfy the conditions expected for an anisotropic gravastar. Certain
energy conditions have been shown to be obeyed and a polytropic equation of
state has been derived. Stability of the solution with respect to possible
axial perturbation is shown to hold.Comment: 19 pages, 9 figures. Latest version contains new and updated
references along with some clarifying remarks in the stability analysi
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
Probing the stability of gravastars by dropping dust shells onto them
As a preparation for the dynamical investigations, this paper begins with a
short review of the three-layer gravastar model with distinguished attention to
the structure of the pertinent parameter space of gravastars in equilibrium.
Then the radial stability of these types of gravastars is studied by
determining their response for the totally inelastic collision of their surface
layer with a dust shell. It is assumed that the dominant energy condition holds
and the speed of sound does not exceed that of the light in the matter of the
surface layer. While in the analytic setup the equation of state is kept to be
generic, in the numerical investigations three functionally distinct classes of
equations of states are applied. In the corresponding particular cases the
maximal mass of the dust shell that may fall onto a gravastar without
converting it into a black hole is determined. For those configurations which
remain stable the excursion of their radius is assigned. It is found that even
the most compact gravastars cannot get beyond the lower limit of the size of
conventional stars, provided that the dominant energy condition holds in both
cases. It is also shown---independent of any assumption concerning the matter
interbridging the internal de Sitter and the external Schwarzschild
regions---that the better is a gravastar in mimicking a black hole the easier
is to get the system formed by a dust shell and the gravastar beyond the event
horizon of the composite system. In addition, a generic description of the
totally inelastic collision of spherical shells in spherically symmetric
spacetimes is also provided in the appendix.Comment: 29 pages, 10 figure
Radial stability analysis of the continuous pressure gravastar
Radial stability of the continuous pressure gravastar is studied using the
conventional Chandrasekhar method. The equation of state for the static
gravastar solutions is derived and Einstein equations for small perturbations
around the equilibrium are solved as an eigenvalue problem for radial
pulsations. Within the model there exist a set of parameters leading to a
stable fundamental mode, thus proving radial stability of the continuous
pressure gravastar. It is also shown that the central energy density possesses
an extremum in rho_c(R) curve which represents a splitting point between stable
and unstable gravastar configurations. As such the rho_c(R) curve for the
gravastar mimics the famous M(R) curve for a polytrope. Together with the
former axial stability calculations this work completes the stability problem
of the continuous pressure gravastar.Comment: 17 pages, 5 figures, References corrected, minor changes wrt v1,
matches published versio
Gravastar energy conditions revisited
We consider the gravastar model where the vacuum phase transition between the
de Sitter interior and the Schwarzschild or Schwarzschild-de Sitter exterior
geometries takes place at a single spherical delta-shell. We derive sharp
analytic bounds on the surface compactness (2m/r) that follow from the
requirement that the dominant energy condition (DEC) holds at the shell. In the
case of Schwarzschild exterior, the highest surface compactness is achieved
with the stiff shell in the limit of vanishing (dark) energy density in the
interior. In the case of Schwarzschild-de Sitter exterior, in addition to the
gravastar configurations with the shell under surface pressure, gravastar
configurations with vanishing shell pressure (dust shells), as well as
configurations with the shell under surface tension, are allowed by the DEC.
Respective bounds on the surface compactness are derived for all cases. We also
consider the speed of sound on the shell as derived from the requirement that
the shell is stable against the radial perturbations. The causality requirement
(sound speed not exceeding that of light) further restricts the space of
allowed gravastar configurations.Comment: LaTeX/IOP-style, 16 pages, 2 figures, changes wrt v1: motivation for
eq. (6) clarified, several referecnes added (to appear in Class. Quantum
Grav.
Dynamics of Logamediate and Intermediate Scenarios in the Dark Energy Filled Universe
We have considered a model of two component mixture i.e., mixture of
Chaplygin gas and barotropic fluid with tachyonic field. In the case, when they
have no interaction then both of them retain their own properties. Let us
consider an energy flow between barotropic and tachyonic fluids. In both the
cases we find the exact solutions for the tachyonic field and the tachyonic
potential and show that the tachyonic potential follows the asymptotic
behavior. We have considered an interaction between these two fluids by
introducing a coupling term. Finally, we have considered a model of three
component mixture i.e., mixture of tachyonic field, Chaplygin gas and
barotropic fluid with or without interaction. The coupling functions decays
with time indicating a strong energy flow at the initial period and weak stable
interaction at later stage. To keep the observational support of recent
acceleration we have considered two particular forms (i) Logamediate Scenario
and (ii) Intermediate Scenario, of evolution of the Universe. We have examined
the natures of the recent developed statefinder parameters and slow-roll
parameters in both scenarios with and without interactions in whole evolution
of the universe.Comment: 28 pages, 20 figure
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