{ "id": "2301.13651", "version": "v1", "published": "2023-01-31T14:09:04.000Z", "updated": "2023-01-31T14:09:04.000Z", "title": "Radio Study of the Pulsar Wind Nebula Powered by PSR B1706-44", "authors": [ "Y. H. Liu", "C. -Y. Ng", "R. Dodson" ], "comment": "16 pages, 9 figures, accepted by APJ", "categories": [ "astro-ph.HE" ], "abstract": "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 (ATCA) 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 $\\sim 0.2c$, 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 semi-circular 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.", "revisions": [ { "version": "v1", "updated": "2023-01-31T14:09:04.000Z" } ], "analyses": { "keywords": [ "pulsar wind nebula", "radio study", "pulsar located inside supernova remnant", "gamma-ray pulsar located inside supernova", "australia telescope compact array" ], "note": { "typesetting": "TeX", "pages": 16, "language": "en", "license": "arXiv", "status": "editable" } } }