109,887 research outputs found
X-ray/GeV emissions from Crab-like pulsars in LMC
We discuss X-ray and gamma-ray emissions from Crab-like pulsars,
PSRs~J0537-6910 and~J0540-6919, in Large Magellanic Cloud. Fermi-LAT
observations have resolved the gamma-ray emissions from these two pulsars and
found the pulsed emissions from PSR~J0540-6919. The total pulsed radiation in
the X-ray/gamma-ray energy bands of PSR~J0540-6919 is observed with the
efficiency (in 4 sr), which is about a factor of
ten larger than of the Crab pulsar. Although
PSR~J0537-6910 has the highest spin-down power among currently known pulsars,
the efficiency of the observed X-ray emissions is about two orders of magnitude
smaller than that of PSR~J0540-6919. This paper mainly discusses what causes
the difference in the radiation efficiencies of these three energetic Crab-like
pulsars. We discuss electron/positron acceleration and high-energy emission
processes within the outer gap model. By solving the outer gap structure with
the dipole magnetic field, we show that the radiation efficiency decreases as
the inclination angle between the magnetic axis and the rotation axis
increases. To explain the difference in the pulse profile and in the radiation
efficiency, our model suggests that PSR~J0540-6919 has an inclination angle
much smaller than the that of Crab pulsar (here we assume the inclination
angles of both pulsars are ). On the other hand, we
speculate that the difference in the radiation efficiencies between
PSRs~J0537-6910 and J0549-6919 is mainly caused by the difference in the Earth
viewing angle, and that we see PSR~J0537-6910 with an Earth viewing angle
(or ) measured from the spin axis, while we
see PSR~J0540-6919 with .Comment: 23 pages, 7 figures, ApJ in pres
Haar expectations of ratios of random characteristic polynomials
We compute Haar ensemble averages of ratios of random characteristic
polynomials for the classical Lie groups K = O(N), SO(N), and USp(N). To that
end, we start from the Clifford-Weyl algebera in its canonical realization on
the complex of holomorphic differential forms for a C-vector space V. From it
we construct the Fock representation of an orthosymplectic Lie superalgebra osp
associated to V. Particular attention is paid to defining Howe's oscillator
semigroup and the representation that partially exponentiates the Lie algebra
representation of sp in osp. In the process, by pushing the semigroup
representation to its boundary and arguing by continuity, we provide a
construction of the Shale-Weil-Segal representation of the metaplectic group.
To deal with a product of n ratios of characteristic polynomials, we let V =
C^n \otimes C^N where C^N is equipped with its standard K-representation, and
focus on the subspace of K-equivariant forms. By Howe duality, this is a
highest-weight irreducible representation of the centralizer g of Lie(K) in
osp. We identify the K-Haar expectation of n ratios with the character of this
g-representation, which we show to be uniquely determined by analyticity, Weyl
group invariance, certain weight constraints and a system of differential
equations coming from the Laplace-Casimir invariants of g. We find an explicit
solution to the problem posed by all these conditions. In this way we prove
that the said Haar expectations are expressed by a Weyl-type character formula
for all integers N \ge 1. This completes earlier work by Conrey, Farmer, and
Zirnbauer for the case of U(N).Comment: LaTeX, 70 pages, Complex Analysis and its Synergies (2016) 2:
Population study for -ray emitting Millisecond Pulsars and unidentified sources
The -LAT has revealed that rotation powered millisecond pulsars (MSPs)
are a major contributor to the Galactic -ray source population. We
discuss the -ray emission process within the context of the outer gap
accelerator model, and use a Monte-Calro method to simulate the Galactic
population of the -ray emitting MSPs. We find that the outer gap
accelerator controlled by the magnetic pair-creation process is preferable in
explaining the possible correlation between the -ray luminosity and the
spin down power. Our Monte-Calro simulation implies that most of the
-ray emitting MSPs are radio quiet in the present sensitivity of the
radio survey, indicating that most of the -ray MSPs have been
unidentified. We argue that the Galactic unidentified sources located
at high latitudes should be dominated by MSPs, whereas the sources in the
galactic plane are dominated by radio-quiet canonical pulsars.Comment: 2011 Fermi Symposium proceedings - eConf C11050
Three-dimensional Two-Layer Outer Gap Model: the Third Peak of Vela Pulsar
We extend the two-dimensional two-layer outer gap model to a
three-dimensional geometry and use it to study the high-energy emission of the
Vela pulsar. We apply this three-dimensional two-layer model to the Vela pulsar
and compare the model light curves, the phase-averaged spectrum and the
phase-resolved spectra with the recent Fermi observations, which also reveals
the existence of the third peak between two main peaks. The phase position of
the third peak moves with the photon energy, which cannot be explained by the
geometry of magnetic field structure and the caustic effect of the photon
propagation. We suggest that the existence of the third peak and its energy
dependent movement results from the azimuthal structure of the outer gap.Comment: 2011 Fermi Symposium proceedings - eConf C11050
Radiation Mechanism of the Soft Gamma-ray Pulsar PSR B1509-58
The outer gap model is used here to explain the spectrum and the energy
dependent light curves of the X-ray and soft gamma-ray radiations of the
spin-down powered pulsar PSR B1509-58.In the outer gap model, most pairs inside
the gap are created around the null charge surface and the gap's electric field
separates the two charges to move in opposite directions. Consequently, the
region from the null charge surface to the light cylinder is dominated by the
outflow of particles and that from the null charge surface to the star is
dominated by the inflow of particles. The inflow and outflow of particles move
along the magnetic field lines and emit curvature photons, and the incoming
curvature photons are converted to pairs by the strong magnetic field of the
star. These pairs emit synchrotron photons. We suggest that the X-rays and soft
gamma-rays of PSR B1509-58 result from the synchrotron radiation of these
pairs, and the viewing angle of PSR B1509-58 only receives the inflow
radiation. The magnetic pair creation requires a large pitch angle, which makes
the pulse profile of the synchrotron radiation distinct from that of the
curvature radiation. We carefully trace the pulse profiles of the synchrotron
radiation with different pitch angles. We find that the differences between the
light curves of different energy bands are due to the different pitch angles of
the secondary pairs, and the second peak appearing at E>10MeV comes from the
region near the star, where the stronger magnetic field allows the pair
creation to happen with a smaller pitch angle.Comment: 5 pages, 8 figures, 2012 Fermi Symposium proceedings - eConf C12102
Possible TeV Source Candidates In The Unidentified EGRET Sources
We study the -ray emission from the pulsar magnetosphere based on
outer gap models, and the TeV radiation from pulsar wind nebulae (PWNe) through
inverse Compton scattering using a one-zone model. We showed previously that
GeV radiation from the magnetosphere of mature pulsars with ages of years old can contribute to the high latitude unidentified EGRET
sources. We carry out Monte Carlo simulations of -ray pulsars in the
Galaxy and the Gould Belt, assuming the pulsar birth rate, initial position,
proper motion velocity, period, and magnetic field distribution and evolution
based on observational statistics. We select from the simulation a sample of
mature pulsars in the Galactic plane () and in the high
latitude () which could be detected by EGRET. The TeV flux from
the pulsar wind nebulae of our simulated sample through the inverse Compton
scattering by relativistic electrons on the microwave cosmic background and
synchrotron seed photons are calculated. The predicted fluxes are consistent
with the present observational constraints. We suggest that strong EGRET
sources can be potential TeV source candidates for present and future
ground-based TeV telescopes.Comment: Minor changes, MNRAS in pres
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