Radio Observation of the Pulsar Wind Nebula in Supernova Remnant G11.2−0.3

Abstract

Pulsar wind nebulae (PWNe) are important sources for understanding galactic high-energy processes, but it is controversial until now how high-energy particles in PWNe are accelerated and transported. Lacking radio counterparts of X-ray PWNe (the proposed acceleration sites) introduces difficulties to better understand questions about multiwavelengths. Our recent 3, 6, and 16 cm high-resolution observations of G11.2−0.3 PWN with the Australia Telescope Compact Array uniquely show morphological similarity with its X-ray PWN (a torus/jet feature). Spectral indices of the radio torus and jet are around −0.09 and −0.10, respectively. Meanwhile, for the jet region, the spectral break between radio and X-ray spectra implies particle acceleration mechanisms other than a diffusive shock acceleration. Polarization results suggest a helical B-field inside the jet, the equipartition B-field strength of which is below 100 μ G.

Keywords

• Pulsar wind nebulae
• Supernova remnants
• Polarimetry