814 research outputs found
Strangeness in Compact Stars and Signal of Deconfinement
Phase transitions in compact stars are discussed including hyperonization,
deconfinement and crystalline phases. Reasons why kaon condensation is unlikely
is reviewed. Particular emphasis is placed on the evolution of internal
structure with spin-down of pulsars. A signature of a first order phase
transition in the timing structure of pulsars which is strong and easy to
measure, is identified.Comment: 17 pages, 15 figures, Latex. (Invited Talk at the International
Symposium on ``Strangeness In Quark Matter 1997'', Thera (Santorini), Hellas,
April 14-18, 1997, To be published in Journal of Physics G (Organizers: A
Panagiotou and J. Madsen
Probing dense matter in neutron stars with axial w-modes
We study the problem of extracting information about composition and equation
of state of dense matter in neutron star interior using axial w-modes. We
determine complex frequencies of axial w-modes for a set of equations of state
involving hyperons as well as Bose-Einstein condensates of antikaons adopting
the continued fraction method. Hyperons and antikaon condensates result in
softer equations of state leading to higher frequencies of first axial w-modes
than that of nuclear matter case, whereas the opposite happens in case of
damping times. The presence of condensates may lead to the appearance of a new
stable branch of superdense stars beyond the neutron star branch called the
third family. The existence of same mass compact stars in both branches are
known as neutron star twins. Further investigation of twins reveal that first
axial w-mode frequencies of superdense stars in the third family are higher
than those of the corresponding twins in the neutron star branch.Comment: LaTeX; 23 pages including two tables and 11 figure
Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down
The conversion of nuclear matter to quark matter in the core of a rotating
neutron star alters its moment of inertia. Hence the epoch over which
conversion takes place will be signaled in the spin-down "signal_prl.tex" 581
lines, 22203 characters characteristics of pulsars. We find that an observable
called the braking index should be easily measurable during the transition
epoch and can have a value far removed (by orders of magnitude) from the
canonical value of three expected for magnetic dipole radiation, and may have
either sign. The duration of the transition epoch is governed by the slow loss
of angular momentum to radiation and is further prolonged by the reduction in
the moment of inertia caused by the phase change which can even introduce an
era of spin-up. We estimate that about one in a hundred pulsars may be passing
through this phase. The phenomenon is analogous to ``bachbending'' observed in
the moment of inertia of rotating nuclei observed in the 1970's, which also
signaled a change in internal structure with changing spin.Comment: 5 pages, 4 figures, Revtex. (May 12, 1997, submitted to PRL
Model study of hot and dense baryonic matter
The properties of baryonic matter have been investigated at finite density
and temperature using different models. The variation of baryon masses and
fractional number densities with baryon density and temperature obtained from
different models have been compared. The quark hadron phase transition have
been studied using Chiral Colour Dieletric (CCD) model in the quark sector. No
phase transition has been seen for the different variants of the
Zimanyi-Moszkowski model. However, a phase transition is observed for the
linear and non-linear Walecka model.Comment: Latex, 16 postscript figures available on reques
Neutron Stars: Recent Developments
Recent developments in neutron star theory and observation are discussed.
Based on modern nucleon-nucleon potentials more reliable equations of state for
dense nuclear matter have been constructed. Furthermore, phase transitions such
as pion, kaon and hyperon condensation, superfluidity and quark matter can
occur in cores of neutron stars. Specifically, the nuclear to quark matter
phase transition and its mixed phases with intriguing structures is treated.
Rotating neutron stars with and without phase transitions are discussed and
compared to observed masses, radii and glitches. The observations of possible
heavy neutron stars in X-ray binaries and QPO's require
relatively stiff equation of states and restrict strong phase transitions to
occur at very high nuclear densities only.Comment: Proc. of the 10th Int. Conf. on Recent Progress in Many-Body Theories
(MBX), Seattle, 10-15 Sep 1999, World Scientific. 16 page
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
Mixed Phase in Compact Starts : M-R relations and radial oscillations
It is believed that quark stars or neutron stars with mixed phase in the core
have smaller radii compared to ordinary compact stars. With the recent
observation of several low radius objects, typically a radius of for
star of mass in low mass X-ray binaries (LMXB), it has become very
important to understand the nature of these objects. An accurate determination
of mass-radius relationship of these objects provide us with a physical
laboratory to study the composition of high density matter and the nature of
phase transition. We study the effect of quark and nuclear matter mixed phase
on mass radius relationship and radial oscillations of neutron stars. We find
that the effect of the mixed phase is to decrease the maximum mass of a stable
neutron star and to decrease the radial frequencies .Comment: guest contribution at Int. Workshop on Astronomy & Relativistic
Astrophysics (IWARA 03)held at Olinda-PE (Brazil) from Oct. 12-17,200
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
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
Universal Charge-Radius Relation for Subatomic and Astrophysical Compact Objects
Electron-positron pair creation in supercritical electric fields limits the
net charge of any static, spherical object, such as superheavy nuclei,
strangelets, and Q-balls, or compact stars like neutron stars, quark stars, and
black holes. For radii between fm and fm the upper bound
on the net charge is given by the universal relation , and for
larger radii (measured in fm or km) . For objects with nuclear density the relation corresponds to
() and (), where is the baryon number. For some systems this
universal upper bound improves existing charge limits in the literature
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