748 research outputs found
Gapless color-flavor locked phase in quark and hybrid stars
We study the effects of the gapless color-flavor locked (gCFL) phase on the
equation of state of strongly interacting matter in the range of baryonic
chemical potential involved in a compact star. We analyze the possibility of a
phase transition from hadronic matter to gCFL quark matter and we discuss, for
different values of the strange quark mass and diquark coupling strength, the
existence of a gCFL phase in quark or hybrid stars. The mass-radius relation
and the structure of compact stars containing the gCFL phase are shown and the
physical relevance of this superconducting phase inside a stellar object is
also discussed.Comment: 7 pages, 11 figure
Decentralization of public-sector agricultural extension in India: The case of the district-level Agricultural Technology Management Agency (ATMA)
agricultural extension reform, Decentralization, demand-driven, organizational capacity,
The influence of medium effects on the gross structure of hybrid stars
We investigate the influence of medium effects on the structure of hybrid
stars, i.e. neutron stars possessing a quark matter core. We found that medium
effects reduce the extent of a pure quark matter phase in the interior of a
hybrid star significantly in favor of a mixed phase of quark and hadronic
matter. Over a wide range of the strong coupling constant - which parameterizes
the influence of medium effects - quark matter is able to exist at least in a
mixed phase in the interior of neutron stars.Comment: 20 pages, LaTeX, 4 inline eps-figures, 4 gif-figures, extended
discussion, to be published in Nucl. Phys. A. Also available at
http://theorie.physik.uni-giessen.de/~schertle/HybSta
Comment on ``Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down''
This is a comment on a paper by Glendenning, Pei, and Weber (Phys. Rev.
Lett., 79, 1603, 1997), where the authors gave an incorrect estimate of the
event rate and neglected the important gravitational energy release. Previous
work on the same subject is reviewed, and a new suggestion is made to link
quark-hadron phase transitions with soft gamma-ray repeaters.Comment: 4 pages; to appear in Phys. Rev. Let
Quark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions
The appearance of quark phases in the dense interior of neutron stars
provides one possibility to soften the equation of state (EOS) of neutron star
matter at high densities. This softening leads to more compact equilibrium
configurations of neutron stars compared to pure hadronic stars of the same
mass. We investigate the question to which amount the compactness of a neutron
star can be attributed to the presence of a quark phase. For this purpose we
employ several hadronic EOS in the framework of the relativistic mean-field
(RMF) model and an extended MIT bag model to describe the quark phase. We find
that - almost independent of the model parameters - the radius of a pure
hadronic neutron star gets typically reduced by 20-30% if a pure quark phase in
the center of the star does exist. For some EOS we furthermore find the
possibility of a "third family" of compact stars which may exist besides the
two known families of white dwarfs and neutron stars. We show how an
experimental proof of the existence of a third family by mass and radius
measurements may provide a unique signature for a phase transition inside
neutron stars.Comment: 37 pages, 18 eps-figures included, LaTe
Neutron spin polarization in strong magnetic fields
The effects of strong magnetic fields on the inner crust of neutron stars are
investigated after taking into account the anomalous magnetic moments of
nucleons. Energy spectra and wave functions for protons and neutrons in a
uniform magnetic field are provided. The particle spin polarizations and the
yields of protons and neutrons are calculated in a free Fermi gas model.
Obvious spin polarization occurs when G for protons and
G for neutrons, respectively. It is shown that the neutron spin
polarization depends solely on the magnetic field strength.Comment: Replaced by the revised version; 10 pages, including 3 eps figure
Tidal effects on magnetic gyration of a charged particle in Fermi coordinates
We examine the gyration motion of a charged particle, viewed from a reference
observer falling along the Z axis into a Schwarzschild black hole. It is
assumed that the magnetic field is constant and uniform along the Z axis, and
that the particle has a circular orbit in the X-Y plane far from the
gravitational source. When the particle as well as the reference observer
approaches the black hole, its orbit is disrupted by the tidal force. The final
plunging velocity increases in the non-relativistic case, but decreases if the
initial circular velocity exceeds a critical value, which is approximately
0.7c. This toy model suggests that disruption of a rapidly rotating star due to
a velocity-dependent tidal force may be quite different from that of a
non-relativistic star. The model also suggested that collapse of the orbit
after the disruption is slow in general, so that the particle subsequently
escapes outside the valid Fermi coordinates.Comment: 10 pages, 12 figure
Structure of Strange Dwarfs with Color Superconducting Core
We study effects of two-flavor color superconductivity on the structure of
strange dwarfs, which are stellar objects with similar masses and radii with
ordinary white dwarfs but stabilized by the strange quark matter core. We find
that unpaired quark matter is a good approximation to the core of strange
dwarfs.Comment: 8 pages 5 figures, J. Phys. G, accepte
Gravitomagnetism in superconductors and compact stars
There are three experimentally observed effects in rotating superconductors
that are so far unexplained. Some authors have tried to interpret such a
phenomena as possible new gravitational properties of coherent quantum systems:
in particular, they suggest that the gravitomagnetic field of that kind of
matter may be many orders of magnitude stronger than the one expected in the
standard theory. Here I show that this interpretation would be in conflict with
the common belief that neutron stars have neutrons in superfluid state and
protons in superconductive one.Comment: 9 pages, no figur
First Order Kaon Condensate
First order Bose condensation in asymmetric nuclear matter and in neutron
stars is studied, with particular reference to kaon condensation. We
demonstrate explicitly why the Maxwell construction fails to assure equilibrium
in multicomponent substances. Gibbs conditions and conservation laws require
that for phase equilibrium, the charge density must have opposite sign in the
two phases of isospin asymmetric nuclear matter. The mixed phase will therefore
form a Coulomb lattice with the rare phase occupying lattice sites in the
dominant phase. Moreover, the kaon condensed phase differs from the normal
phase, not by the mere presence of kaons in the first, but also by a difference
in the nucleon effective masses. The mixed phase region, which occupies a large
radial extent amounting to some kilometers in our model neutron stars, is thus
highly heterogeneous. It should be particularly interesting in connection with
the pulsar glitch phenomenon as well as transport properties.Comment: 25 pagees, 20 figures, Late
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