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Post Info TOPIC: PSR J0835-4510
Blobrana


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Posts: 131433
Date:
Vela Pulsar
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ATel 9847: Glitch observed in the Vela Pulsar (PSR J0835-4510)



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Blobrana


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Posts: 131433
Date:
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The star of this movie is the Vela pulsar, a neutron star that was formed when a massive star collapsed. The Vela pulsar is about 1,000 light years from Earth, spans is about 12 miles in diameter, and makes over 11 complete rotations every second, faster than a helicopter rotor. As the pulsar whips around, it spews out a jet of charged particles that race out along the pulsars rotation axis at about 70% of the speed of light.
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Blobrana


L

Posts: 131433
Date:
PSR J0835-4510
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Title: The helical jet of the Vela Pulsar
Authors: Martin Durant, Oleg Kargaltsev, George G. Pavlov, Julia Kropotina, Kseniya Levenfish

We have studied the fascinating dynamics of the nearby Vela pulsar's nebula in a campaign comprising eleven 40ks observations with Chandra X-ray Observatory (CXO). The deepest yet images revealed the shape, structure, and motion of the 2-arcminute-long pulsar jet. We find that the jet's shape and dynamics are remarkably consistent with that of a steadily turning helix projected on the sky. We discuss possible implications of our results, including free precession of the neutron star and MHD instability scenarios.

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Blobrana


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Posts: 131433
Date:
Vela X
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Title: Escape from Vela X
Authors: James Hinton, Stefan Funk, Robert Parsons, Stefan Ohm

Whilst the Vela pulsar and its associated nebula are often considered as the archetype of a system powered by a ~10^4 year old isolated neutron star, many features of the spectral energy distribution of this pulsar wind nebula are both puzzling and unusual. Here we develop a model that for the first time relates the main structures in the system, the extended radio nebula (ERN) and the X-ray cocoon through continuous injection of particles with a fixed spectral shape. We argue that diffusive escape of particles from the ERN can explain the steep Fermi-LAT spectrum. In this scenario Vela X should produce a distinct feature in the locally-measured cosmic ray electron spectrum at very high energies. This prediction can be tested in the future using the Cherenkov Telescope Array (CTA). If particles are indeed released early in the evolution of PWNe and can avoid severe adiabatic losses, PWN provide a natural explanation for the rising positron fraction in the local CR spectrum.

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