11,758 research outputs found
Dense matter equation of state for neutron star mergers
In simulations of binary neutron star mergers, the dense matter equation of
state (EOS) is required over wide ranges of density and temperature as well as
under conditions in which neutrinos are trapped, and the effects of magnetic
fields and rotation prevail. Here we assess the status of dense matter theory
and point out the successes and limitations of approaches currently in use. A
comparative study of the excluded volume (EV) and virial approaches for the
system using the equation of state of Akmal, Pandharipande and
Ravenhall for interacting nucleons is presented in the sub-nuclear density
regime. Owing to the excluded volume of the -particles, their mass
fraction vanishes in the EV approach below the baryon density 0.1 fm,
whereas it continues to rise due to the predominantly attractive interactions
in the virial approach. The EV approach of Lattimer et al. is extended here to
include clusters of light nuclei such as d, H and He in addition to
-particles. Results of the relevant state variables from this
development are presented and enable comparisons with related but slightly
different approaches in the literature. We also comment on some of the sweet
and sour aspects of the supra-nuclear EOS. The extent to which the neutron star
gravitational and baryon masses vary due to thermal effects, neutrino trapping,
magnetic fields and rotation are summarized from earlier studies in which the
effects from each of these sources were considered separately. Increases of
about occur for rigid (differential) rotation with
comparable increases occurring in the presence of magnetic fields only for
fields in excess of Gauss. Comparatively smaller changes occur due to
thermal effects and neutrino trapping. Some future studies to gain further
insight into the outcome of dynamical simulations are suggested.Comment: Revised manuscript with one additional figure and previous Fig. 4
replaced, 19 additional references and new tex
Pulsar Kicks With Modified URCA and Electrons in Landau Levels
We derive the energy asymmetry given the proto-neutron star during the time
when the neutrino sphere is near the surface of the proto-neutron star, using
the modified URCA process. The electrons produced with the anti-neutrinos are
in Landau levels due to the strong magnetic field, and this leads to asymmetry
in the neutrino momentum, and a pulsar kick. The magnetic field must be strong
enough for a large fraction of the eletrons to be in the lowest Landau level,
however, there is no direct dependence of our pulsar velocity on the strength
of the magnetic field. Our main prediction is that the large pulsar kicks start
at about 10 s and last for about 10 s, with the corresponding neutrinos
correlated in the direction of the magnetic field. We predict a pulsar velocity
of 1.03 km/s, which reaches 1000 km/s if T
K.Comment: 11 pages, 6 figure
Evolution of Proto-Neutron stars with kaon condensates
We present simulations of the evolution of a proto-neutron star in which
kaon-condensed matter might exist, including the effects of finite temperature
and trapped neutrinos. The phase transition from pure nucleonic matter to the
kaon condensate phase is described using Gibbs' rules for phase equilibrium,
which permit the existence of a mixed phase. A general property of neutron
stars containing kaon condensates, as well as other forms of strangeness, is
that the maximum mass for cold, neutrino-free matter can be less than the
maximum mass for matter containing trapped neutrinos or which has a finite
entropy. A proto-neutron star formed with a baryon mass exceeding that of the
maximum mass of cold, neutrino-free matter is therefore metastable, that is, it
will collapse to a black hole at some time during the Kelvin-Helmholtz cooling
stage.
The effects of kaon condensation on metastable stars are dramatic. In these
cases, the neutrino signal from a hypothetical galactic supernova (distance
kpc) will stop suddenly, generally at a level above the background in
the SuperK and SNO detectors, which have low energy thresholds and backgrounds.
This is in contrast to the case of a stable star, for which the signal
exponentially decays, eventually disappearing into the background. We find the
lifetimes of kaon-condensed metastable stars to be restricted to the range
40--70 s and weakly dependent on the proto-neutron star mass, in sharp contrast
to the significantly larger mass dependence and range (1--100 s) of
hyperon-rich metastable stars.Comment: 25 pages, 14 figures. Submitted to Astrophysical Journa
Two-Hop Routing with Traffic-Differentiation for QoS Guarantee in Wireless Sensor Networks
This paper proposes a Traffic-Differentiated Two-Hop Routing protocol for
Quality of Service (QoS) in Wireless Sensor Networks (WSNs). It targets WSN
applications having different types of data traffic with several priorities.
The protocol achieves to increase Packet Reception Ratio (PRR) and reduce
end-to-end delay while considering multi-queue priority policy, two-hop
neighborhood information, link reliability and power efficiency. The protocol
is modular and utilizes effective methods for estimating the link metrics.
Numerical results show that the proposed protocol is a feasible solution to
addresses QoS service differenti- ation for traffic with different priorities.Comment: 13 page
Wigner's -matrix elements for - A Generating Function Approach
A generating function for the Wigner's -matrix elements of is
derived. From this an explicit expression for the individual matrix elements is
obtained in a closed form.Comment: RevTex 3.0, 22 pages, no figure
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