1,734 research outputs found
Phase Structure of Compact Star in Modified Quark-Meson Coupling Model
The K condensation and quark deconfinement phase transitions are
investigated in the modified quark-meson coupling model. It is shown that K
condensation is suppressed because of the quark deconfinement when
202.2MeV, where is the bag constant for unpaired quark matter.
With the equation of state (EOS) solved self-consistently, we discuss the
properties of compact stars. We find that the EOS of pure hadron matter with
condensed K phase should be ruled out by the redshift for star EXO0748-676,
while EOS containing unpaired quark matter phase with being about
180MeV could be consistent with this observation and the best measured mass of
star PSR 1913+16. We then probe into the change of the phase structures in
possible compact stars with deconfinment phase as the central densities
increase. But if the recent inferred massive star among Terzan 5 with
M1.68M is confirmed, all the present EOSes with condensed phase
and deconfined phase would be ruled out and therefore these exotic phases are
unlikely to appear within neutron stars.Comment: 11 pages, 5 figure
A CLEAN-based Method for Deconvolving Interstellar Pulse Broadening from Radio Pulses
Multipath propagation in the interstellar medium distorts radio pulses, an
effect predominant for distant pulsars observed at low frequencies. Typically,
broadened pulses are analyzed to determine the amount of propagation-induced
pulse broadening, but with little interest in determining the undistorted pulse
shapes. In this paper we develop and apply a method that recovers both the
intrinsic pulse shape and the pulse broadening function that describes the
scattering of an impulse. The method resembles the CLEAN algorithm used in
synthesis imaging applications, although we search for the best pulse
broadening function, and perform a true deconvolution to recover intrinsic
pulse structre. As figures of merit to optimize the deconvolution, we use the
positivity and symmetry of the deconvolved result along with the mean square
residual and the number of points below a given threshold. Our method makes no
prior assumptions about the intrinsic pulse shape and can be used for a range
of scattering functions for the interstellar medium. It can therefore be
applied to a wider variety of measured pulse shapes and degrees of scattering
than the previous approaches. We apply the technique to both simulated data and
data from Arecibo observations.Comment: 9 pages, 6 figures, Accepted for publication in the Astrophysical
Journa
Extracting the three- and four-graviton vertices from binary pulsars and coalescing binaries
Using a formulation of the post-Newtonian expansion in terms of Feynman
graphs, we discuss how various tests of General Relativity (GR) can be
translated into measurement of the three- and four-graviton vertices. In
problems involving only the conservative dynamics of a system, a deviation of
the three-graviton vertex from the GR prediction is equivalent, to lowest
order, to the introduction of the parameter beta_{PPN} in the parametrized
post-Newtonian formalism, and its strongest bound comes from lunar laser
ranging, which measures it at the 0.02% level. Deviation of the three-graviton
vertex from the GR prediction, however, also affects the radiative sector of
the theory. We show that the timing of the Hulse-Taylor binary pulsar provides
a bound on the deviation of the three-graviton vertex from the GR prediction at
the 0.1% level. For coalescing binaries at interferometers we find that,
because of degeneracies with other parameters in the template such as mass and
spin, the effects of modified three- and four-graviton vertices is just to
induce an error in the determination of these parameters and, at least in the
restricted PN approximation, it is not possible to use coalescing binaries for
constraining deviations of the vertices from the GR prediction.Comment: 10 pages, 5 figures; v2: an error corrected; references adde
Detection of OH absorption against PSR B1849+00
We have searched for OH absorption against seven pulsars using the Arecibo
telescope. In both OH mainlines (at 1665 and 1667 MHz), deep and narrow
absorption features were detected toward PSR B1849+00. In addition, we have
detected several absorption and emission features against B33.6+0.1, a nearby
supernova remnant (SNR). The most interesting result of this study is that a
pencil-sharp absorption sample against the PSR differs greatly from the
large-angle absorption sample observed against the SNR. If both the PSR and the
SNR probe the same molecular cloud then this finding has important implications
for absorption studies of the molecular medium, as it shows that the statistics
of absorbing OH depends on the size of the background source. We also show that
the OH absorption against the PSR most likely originates from a small (<30
arcsec) and dense (>10^5 cm^-3) molecular clump.Comment: 12 pages, 8 figures. Accepted for publication in Ap
A post-Keplerian parameter to test gravito-magnetic effects in binary pulsar systems
We study the pulsar timing, focusing on the time delay induced by the
gravitational field of the binary systems. In particular, we study the
gravito-magnetic correction to the Shapiro time delay in terms of Keplerian and
post-Keplerian parameters, and we introduce a new post-Keplerian parameter
which is related to the intrinsic angular momentum of the stars. Furthermore,
we evaluate the magnitude of these effects for the binary pulsar systems known
so far. The expected magnitude is indeed small, but the effect is important per
se.Comment: 6 pages, RevTeX, 1 eps figure, accepted for publication in Physical
Review D; references adde
A Modified Scalar-Tensor-Vector Gravity Theory and the Constraint on its Parameters
A gravity theory called scalar-tensor-vector gravity (STVG) has been recently
developed and succeeded in solar system, astrophysical and cosmological scales
without dark matter [J. W. Moffat, J. Cosmol. Astropart. Phys. 03, 004 (2006)].
However, two assumptions have been used: (i) , where and
are and in the Schwarzschild coordinates (static and
spherically symmetric); (ii) scalar field in the solar system. These
two assumptions actually imply that the standard parametrized post-Newtonian
parameter . In this paper, we relax these two assumptions and study
STVG further by using the post-Newtonian (PN) approximation approach. With
abandoning the assumptions, we find in general cases of STVG.
Then, a version of modified STVG (MSTVG) is proposed through introducing a
coupling function of scalar field G: . We have derived the metric
and equations of motion (EOM) in 1PN for general matter without specific
equation of state and point masses firstly. Subsequently, the secular
periastron precession of binary pulsars in harmonic coordinates
is given. After discussing two PPN parameters ( and ) and two
Yukawa parameters ( and ), we use of four
binary pulsars data (PSR B1913+16, PSR B1534+12, PSR J0737-3039 and PSR
B2127+11C) to constrain the Yukawa parameters for MSTVG:
m and if
we fix .Comment: 39 pages, 4 figures, accepted by PR
The Madison plasma dynamo experiment: a facility for studying laboratory plasma astrophysics
The Madison plasma dynamo experiment (MPDX) is a novel, versatile, basic
plasma research device designed to investigate flow driven magnetohydrodynamic
(MHD) instabilities and other high- phenomena with astrophysically
relevant parameters. A 3 m diameter vacuum vessel is lined with 36 rings of
alternately oriented 4000 G samarium cobalt magnets which create an
axisymmetric multicusp that contains 14 m of nearly magnetic field
free plasma that is well confined and highly ionized . At present, 8
lanthanum hexaboride (LaB) cathodes and 10 molybdenum anodes are inserted
into the vessel and biased up to 500 V, drawing 40 A each cathode, ionizing a
low pressure Ar or He fill gas and heating it. Up to 100 kW of electron
cyclotron heating (ECH) power is planned for additional electron heating. The
LaB cathodes are positioned in the magnetized edge to drive toroidal
rotation through torques that propagate into the
unmagnetized core plasma. Dynamo studies on MPDX require a high magnetic
Reynolds number , and an adjustable fluid Reynolds number , in the regime where the kinetic energy of the flow exceeds the magnetic
energy (vv). Initial results from MPDX are presented
along with a 0-dimensional power and particle balance model to predict the
viscosity and resistivity to achieve dynamo action.Comment: 14 pages, 13 figure
Vainshtein Mechanism in Binary Pulsars
We compute the scalar gravitational radiation from a binary pulsar system in
the simplest model that exhibits the Vainshtein mechanism. The mechanism is
successful in screening the effect from scalar fields conformally coupled to
matter, although gravitational radiation is less suppressed relative to its
general relativity predictions than static fifth forces effects within the
pulsar system. This is due to a combination of two effects: firstly the
existence of monopole and dipole radiation; secondly the Vainshtein suppression
comes from the hierarchy of scales between the inverse frequency scale and the
Vainshtein radius, rather than the orbital radius of the pulsar system.
Extensions of these results will have direct relevance to infrared
modifications of gravity, such as massive gravity theories, which are known to
exhibit a Vainshtein mechanism. Generalization to Galileon models with higher
order interactions are likely to provide stronger constraints.Comment: minor revisions to match published version in pr
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