71,726 research outputs found
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
Long-term X-ray emission from Swift J1644+57
The X-ray emission from Swift J1644+57 is not steadily decreasing instead it
shows multiple pulses with declining amplitudes. We model the pulses as reverse
shocks from collisions between the late ejected shells and the externally
shocked material, which is decelerated while sweeping the ambient medium. The
peak of each pulse is taken as the maximum emission of each reverse shock. With
a proper set of parameters, the envelope of peaks in the light curve as well as
the spectrum can be modelled nicely.Comment: 6 pages, 2 figures, accepted for publication in MNRA
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
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