Multi-zone Modeling of the Pulsar Wind Nebula HESS J1825-137

Details Multi-zone Modeling of the Pulsar Wind Nebula HESS J1825-137 Multi-zone Modeling of the Pulsar Wind Nebula HESS J1825-137

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...742...62v&link_type=abstract

The Astrophysical Journal, Volume 742, Issue 2, article id. 62 (2011).

Astronomy and Astrophysics

Astronomy

2

Pulsars: Individual: Psr J1826–1334, X-Rays: General

Scientific paper

The pulsar wind nebula associated with PSR J1826-1334, HESS J1825-137, is a bright very high energy (VHE) source with an angular extent of ~1° and spatially resolved spectroscopic TeV measurements. The gamma-ray spectral index is observed to soften with increasing distance from the pulsar, likely the result of cooling losses as electrons traverse the nebula. We describe analysis of X-ray data of the extended nebula, as well as three-dimensional time-dependent spectral energy distribution modeling, with emphasis on the spatial variations within HESS J1825-137. The multi-wavelength data place significant constraints on electron injection, transport, and cooling within the nebula. The large size and high nebular energy budget imply a relatively rapid initial pulsar spin period of 13 ± 7 ms and an age of 40 ± 9 kyr. The relative fluxes of each VHE zone can be explained by advective particle transport with a radially decreasing velocity profile with v(r)vpropr -0.5. The evolution of the cooling break requires an evolving magnetic field which also decreases radially from the pulsar, B(r,t) \propto r^{-0.7} \, \dot{E}(t)^{1/2}. Detection of 10 TeV flux ~80 pc from the pulsar requires rapid diffusion of high-energy particles with \tau _{esc} \approx 90 \, (R / 10 \, {pc})^2 ({\it E_e}/100 \, {TeV})^{-1} \, {year}, contrary to the common assumption of toroidal magnetic fields with strong magnetic confinement. The model predicts a rather uniform Fermi Large Area Telescope (LAT) surface brightness out to ~1° from the pulsar, in good agreement with the recently discovered LAT source centered 0fdg5 southwest of PSR J1826-1334 with extension 0fdg6 ± 0fdg1.

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