Escape from Vela X

Abstract

Whilst the Vela pulsar and its associated nebula are often considered as the archetype of a system powered by a \sim10^4 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.

Accepted for publication in Astrophysical Journal Letters

References in corpus (8)

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• The ATNF Pulsar Catalogue
• First detection of a VHE gamma-ray spectral maximum from a Cosmic source: H.E.S.S. discovery of the Vela X nebula
• A Dynamical Model for the Evolution of a Pulsar Wind Nebula inside a Non-Radiative Supernova Remnant
• A Cosmic Ray Positron Anisotropy due to Two Middle-Aged, Nearby Pulsars?
• Inverse Compton Scenarios for the TeV Gamma-Ray Emission of the Galactic Centre
• Probing the radio to X-ray connection of the Vela X PWN with Fermi LAT and H.E.S.S
• Estimating the birth period of pulsars through GLAST/LAT observations of their wind nebulae

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