529 research outputs found
Thermal Evolution of a Pulsating Neutron Star
We have derived a set of equations to describe the thermal evolution of a
neutron star which undergoes small-amplitude radial pulsations. We have taken
into account, in the frame of the General Theory of Relativity, the pulsation
damping due to the bulk and shear viscosity and the accompanying heating of the
star. The neutrino emission of a pulsating non-superfluid star and its heating
due to the bulk viscosity are calculated assuming that both processes are
determined by the non-equilibrium modified Urca process. Analytical and
numerical solutions to the set of equations of the stellar evolution are
obtained for linear and strongly non-linear deviations from beta-equilibrium.
It is shown that a pulsating star may be heated to very high temperatures,
while the pulsations damp very slowly with time (a power law damping for
100-1000 years), as long as the damping is determined by the bulk viscosity.
The contribution of the shear viscosity to the damping becomes important in a
rather cool star with a low pulsation energy.Comment: 10 pages, 3 figures, an important reference to the paper by Finzi &
Wolf (1968) is added; analytical consideration of the problem (Section 5) is
essentially extende
Spatial and Wavenumber Resolution of Doppler Reflectometry
Doppler reflectometry spatial and wavenumber resolution is analyzed within
the framework of the linear Born approximation in slab plasma model. Explicit
expression for its signal backscattering spectrum is obtained in terms of
wavenumber and frequency spectra of turbulence which is assumed to be radially
statistically inhomogeneous. Scattering efficiency for both back and forward
scattering (in radial direction) is introduced and shown to be inverse
proportional to the square of radial wavenumber of the probing wave at the
fluctuation location thus making the spatial resolution of diagnostics
sensitive to density profile. It is shown that in case of forward scattering
additional localization can be provided by the antenna diagram. It is
demonstrated that in case of backscattering the spatial resolution can be
better if the turbulence spectrum at high radial wavenumbers is suppressed. The
improvement of Doppler reflectometry data localization by probing beam focusing
onto the cut-off is proposed and described. The possibility of Doppler
reflectometry data interpretation based on the obtained expressions is shown.Comment: http://stacks.iop.org/0741-3335/46/114
Cooling of Akmal-Pandharipande-Ravenhall neutron star models
We study the cooling of superfluid neutron stars whose cores consist of
nucleon matter with the Akmal-Pandharipande-Ravenhall equation of state. This
equation of state opens the powerful direct Urca process of neutrino emission
in the interior of most massive neutron stars. Extending our previous studies
(Gusakov et al. 2004a, Kaminker et al. 2005), we employ phenomenological
density-dependent critical temperatures T_{cp}(\rho) of strong singlet-state
proton pairing (with the maximum T_{cp}^{max} \sim 7e9 K in the outer stellar
core) and T_{cnt}(\rho) of moderate triplet-state neutron pairing (with the
maximum T_{cnt}^{max} \sim 6e8 K in the inner core). Choosing properly the
position of T_{cnt}^{max} we can obtain a representative class of massive
neutron stars whose cooling is intermediate between the cooling enhanced by the
neutrino emission due to Cooper pairing of neutrons in the absence of the
direct Urca process and the very fast cooling provided by the direct Urca
process non-suppressed by superfluidity.Comment: 9 pages, 6 figures; accepted for publication in MNRA
Enhanced cooling of neutron stars via Cooper-pairing neutrino emission
We simulate cooling of superfluid neutron stars with nucleon cores where
direct Urca process is forbidden. We adopt density dependent critical
temperatures and of singlet-state proton and
triplet-state neutron pairing in a stellar core and consider a strong proton
pairing (with maximum T_{cp}^{max} \ga 5 \times 10^9 K) and a moderate
neutron pairing ( K). When the internal
stellar temperature falls below , the neutrino luminosity
due to Cooper pairing of neutrons behaves , just as that
produced by modified Urca process (in a non-superfluid star) but is higher by
about two orders of magnitude. In this case the Cooper-pairing neutrino
emission acts like an enhanced cooling agent. By tuning the density dependence
we can explain observations of cooling isolated neutron stars in
the scenario in which direct Urca process or similar process in kaon/pion
condensed or quark matter are absent.Comment: 9 pages, 3 figures, submitted to A&
Direct Urca Process in a Neutron Star Mantle
We show that the direct Urca process of neutrino emission is allowed in two
possible phases of nonspherical nuclei (inverse cylinders and inverse spheres)
in the mantle of a neutron star near the crust-core interface. The process is
open because neutrons and protons move in a periodic potential created by
inhomogeneous nuclear structures. In this way the nucleons acquire large
quasimomenta needed to satisfy momentum-conservation in the neutrino reaction.
The appropriate neutrino emissivity in a nonsuperfluid matter is about 2--3
orders of magnitude higher than the emissivity of the modified Urca process in
the stellar core. The process may noticeably accelerate the cooling of low-mass
neutron stars.Comment: 7 pages, 3 figures, submitted to A&
Anomalies in Superfluids and a Chiral Electric Effect
We analyze the chiral transport terms in relativistic superfluid
hydrodynamics. In addition to the spontaneously broken symmetry current, we
consider an arbitrary number of unbroken symmetries and extend the results of
arXiv:1105.3733. We suggest an interpretation of some of the new transport
coefficients in terms of chiral and gravitational anomalies. In particular, we
show that with unbroken gauged charges in the system, one can observe a chiral
electric conductivity - a current in a perpendicular direction to the applied
electric field. We present a motivated proposal for the value of the associated
transport coefficient, linking it to the triangle anomaly. Along the way we
present new arguments regarding the interpretation of the anomalous transport
coefficients in normal fluids. We propose a natural generalization of the
chiral transport terms to the case of an arbitrary number of spontaneously
broken symmetry currents.Comment: 30 pages; v2: Onsager-relations argument corrected, references added;
v3: fixed missing line in eq. (38
Magnetars as cooling neutron stars with internal heating
We study thermal structure and evolution of magnetars as cooling neutron
stars with a phenomenological heat source in a spherical internal layer. We
explore the location of this layer as well as the heating rate that could
explain high observable thermal luminosities of magnetars and would be
consistent with the energy budget of neutron stars. We conclude that the heat
source should be located in an outer magnetar's crust, at densities rho < 5e11
g/cm^3, and should have the heat intensity of the order of 1e20 erg/s/cm^3.
Otherwise the heat energy is mainly emitted by neutrinos and cannot warm up the
surface.Comment: 8 pages, 5 figures, submitted to MNRA
Cooling of Neutron Stars: Two Types of Triplet Neutron Pairing
We consider cooling of neutron stars (NSs) with superfluid cores composed of
neutrons, protons, and electrons (assuming singlet-state pairing of protons,
and triplet-state pairing of neutrons). We mainly focus on (nonstandard)
triplet-state pairing of neutrons with the projection of the total
angular momentum of Cooper pairs onto quantization axis. The specific feature
of this pairing is that it leads to a power-law (nonexponential) reduction of
the emissivity of the main neutrino processes by neutron superfluidity. For a
wide range of neutron critical temperatures , the cooling of NSs with
the superfluidity is either the same as the cooling with the superfluidity, considered in the majority of papers, or much faster. The
cooling of NSs with density dependent critical temperatures and
can be imitated by the cooling of the NSs with some effective
critical temperatures and constant over NS cores. The
hypothesis of strong neutron superfluidity with is inconsistent
with current observations of thermal emission from NSs, but the hypothesis of
weak neutron superfluidity of any type does not contradict to observations.Comment: 10 pages, 6 figure
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