Non-thermal emission from Vela X and PWN G0.9+0.1

Details Non-thermal emission from Vela X and PWN G0.9+0.1 Non-thermal emission from Vela X and PWN G0.9+0.1

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009raa.....9..449q&link_type=abstract

Research in Astronomy and Astrophysics, Volume 9, Issue 4, pp. 449-456 (2009).

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

We study the multi-waveband non-thermal emission from the pulsar wind nebulae (PWNe) Vela X and G0.9 + 0.1 in the frame of a time-dependent model describing non-thermal radiation from the PWNe. In such a model, the relativistic wind of particles driven by a central pulsar blows into the ambient medium and creates a termination shock that accelerates the particles to very high energy in a PWN. The non-thermal photons in the PWN are produced both by synchrotron radiation and the inverse Compton process, with electrons coming directly from the pulsar magnetosphere and electrons being accelerated at the termination shock. We apply this model to reproduce the observed multi-waveband photon spectra of Vela X and the G0.9+0.1, both of which have been detected emitting very high energy photons. Our results indicate that TeV photons are produced by the inverse Compton scattering of the high-energy electrons in the infrared photon field in both Vela X and PWN G0.9+0.1. The TeV photons from these two PWNe may have leptonic origins.

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