2,634 research outputs found
Pulsar Signal of Deconfinement
A solitary millisecond pulsar, if near the mass limit, and undergoing a phase
transition, either first or second order, provided the transition is to a
substantially more compressible phase, will emit a blatantly obvious
signal---spontaneous spin-up. Normally a pulsar spins down by angular momentum
loss to radiation. The signal is trivial to detect and is estimated to be
``on'' for 1/50 of the spin-down era of millisecond pulsars. Presently about 25
solitary millisecond pulsars are known. The phenomenon is analogous to
``backbending'' observed in high spin nuclei in the 1970's.Comment: 12 pages, 11 figures, Latex-espcrc1.sty (Dec. 1997, Plenary Talk to
appear in Nuclear Physics A in the Proceedings of Quark Matter97, Tsukuba,
Japan
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
Mapping Deconfinement with a Compact Star Phase Diagram
We have found correlations between properties of the equation of state for
stellar matter with a phase transition at supernuclear densities and two
characteristic features of a "phase diagram" for rotating compact stars in the
angular velocity - baryon number plane: 1) the critical dividing line between
mono- and two-phase star configurations and 2) the maximum mass line. The
second line corresponds to the minimum mass function for black hole candidates
whereas the first one is observable by a population statistics, e.g. for
Z-sources in low-mass X-ray binaries. The observation of a population gap in
the mass distribution for the latter is suggested as an astrophysical
verification of the existence of a first order phase transition in QCD at high
densities such as the deconfinement.Comment: 4 pages, 2 figures, Contribution to Proceedings of Quark Matter 2002,
Nantes, July 18 - 24, 200
Surface Tension between Kaon Condensate and Normal Nuclear Matter Phase
We calculate for the first time the surface tension and curvature coefficient
of a first order phase transition between two possible phases of cold nuclear
matter, a normal nuclear matter phase in equilibrium with a kaon condensed
phase, at densities a few times the saturation density. We find the surface
tension is proportional to the difference in energy density between the two
phases squared. Furthermore, we show the consequences for the geometrical
structures of the mixed phase region in a neutron star.Comment: 7 pages, 5 figures (Latex
From Quark Stars to Hybrid Stars
We show the possible existence of compact stars having a surface composed of
a mixed phase of quarks and hadrons. This scenario can be realized both for
self-bound stars, satisfying the so-called Witten-Bodmer hypothesis, and for
gravitationally bound stars. This class of solutions of the
Tolman-Oppenheimer-Volkoff equation can be obtained in all the models we
discuss, within a physically acceptable range of values of the model
parameters.Comment: 10 pages, 4 figures, 1 tabl
Spin-up of the hyperon-softened accreting neutron stars
We study the spin-up of the accreting neutron stars with a realistic
hyperon-softened equation of state. Using precise 2-D calculations we study the
evolutionary tracks of accreting neutron stars in the angular-momentum -
frequency plane. In contrast to the case of spinning-down solitary
radio-pulsars, where a strong back-bending behavior has been observed, we do
not see back-bending phenomenon in the accretion-powered spinning-up case. We
conclude that in the case of accretion-driven spin-up the back-bending is
strongly suppressed by the mass-increase effect accompanying the
angular-momentum increase.Comment: 5 pages, 5 figures, accepted by Astronomy & Astrophysic
Kaon Condensation in Neutron Star Matter with Hyperons
Based on the Kaplan-Nelson Lagrangian, we investigate kaon condensation in
dense neutron star matter allowing for the explicit presence of hyperons. Using
various models we find that the condensate threshold is sensitive to the
behavior of the scalar density; the more rapidly it increases with baryon
density, the lower is the threshold for condensation. The presence of hyperons,
particularly the , shifts the threshold for condensation to a
higher density. In the mean field approach, with hyperons, the condensate
amplitude grows sufficiently rapidly that the nucleon effective mass vanishes
at a finite density and a satisfactory treatment of the thermodynamics cannot
be achieved. Thus, calculations of kaon-baryon interactions beyond the mean
field level appear to be necessary.Comment: 13 pages, latex, 3 figures by fax/mail from [email protected]
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