Radio Study of the Pulsar Wind Nebula Powered by PSR B1706-44

Y. H. Liu, C. Y. Ng, R. Dodson

Research output: Contribution to journalArticlepeer-review


PSR B1706−44 is an energetic gamma-ray pulsar located inside supernova remnant (SNR) G343.1−2.3 and it powers a compact pulsar wind nebula (PWN) that shows torus and jet structure in X-rays. We present a radio study of the PWN using Australia Telescope Compact Array observations at 3, 6, 13, and 21 cm. We found an overall arc-like morphology at 3 and 6 cm, and the “arc” shows two distinct peaks at 6 cm. The radio emission is faint inside the X-ray PWN and only brightens beyond that. We develop a thick torus model with Doppler boosting effect to explain the radio PWN structure. The model suggests a bulk flow speed of ∼0.2c, which could indicate significant deceleration of the flow from the X-ray emitting region. Our polarization result reveals a highly ordered toroidal B field in the PWN. Its origin is unclear given that the supernova reverse shock should have interacted with the PWN. At a larger scale, the 13 and 21 cm radio images detected a semicircular rim and an east-west ridge of G343.1−2.3. We argue that the latter could possibly be a pulsar tail rather than a filament of the SNR, as supported by the flat radio spectrum and the alignment between the magnetic field and its elongation.

Original languageEnglish
Article number82
JournalAstrophysical Journal
Issue number1
Publication statusPublished - 1 Mar 2023


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