Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/139418
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dc.contributor.author | Anderson, G.E. | - |
dc.contributor.author | Russell, T.D. | - |
dc.contributor.author | Fausey, H.M. | - |
dc.contributor.author | van der Horst, A.J. | - |
dc.contributor.author | Hancock, P.J. | - |
dc.contributor.author | Bahramian, A. | - |
dc.contributor.author | Bell, M.E. | - |
dc.contributor.author | Miller-Jones, J.C.A. | - |
dc.contributor.author | Rowell, G. | - |
dc.contributor.author | Sammons, M.W. | - |
dc.contributor.author | Wijers, R.A.M.J. | - |
dc.contributor.author | Galvin, T.J. | - |
dc.contributor.author | Goodwin, A.J. | - |
dc.contributor.author | Konno, R. | - |
dc.contributor.author | Rowlinson, A. | - |
dc.contributor.author | Ryder, S.D. | - |
dc.contributor.author | Schüssler, F. | - |
dc.contributor.author | Wagner, S.J. | - |
dc.contributor.author | Zhu, S.J. | - |
dc.date.issued | 2023 | - |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2023; 523(4):4992-5005 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.issn | 1365-2966 | - |
dc.identifier.uri | https://hdl.handle.net/2440/139418 | - |
dc.description.abstract | We observed the rapid radio brightening of GRB 210702A with the Australia Telescope Compact Array (ATCA) just 11 h post-burst, tracking early-time radio variability over a 5 h period on ∼15 min time-scales at 9.0, 16.7, and 21.2 GHz. A broken power law fit to the 9.0 GHz light curve showed that the 5 h flare peaked at a flux density of 0.4 ± 0.1 mJy at ∼13 h post-burst. The observed temporal and spectral evolution is not expected in the standard internal–external shock model, where forward and reverse shock radio emission evolves on much longer time-scales. The early-time (<1 d) optical and X-ray light curves from the Neil Gehrels Swift Observatory demonstrated typical afterglow forward shock behaviour, allowing us to use blast wave physics to determine a likely homogeneous circumburst medium and an emitting electron population power-law index of p = 2.9 ± 0.1. We suggest that the early-time radio flare is likely due to weak interstellar scintillation (ISS), which boosted the radio afterglow emission above the ATCA sensitivity limit on minute time-scales. Using relations for ISS in the weak regime, we were able to place an upper limit on the size of the blast wave of ≲6 × 1016 cm in the plane of the sky, which is consistent with the theoretical forward shock size prediction of 8 × 1016 cm for GRB 210702A at ∼13 h post-burst. This represents the earliest ISS size constraint on a gamma-ray burst (GRB) blast wave to date, demonstrating the importance of rapid (<1 d) radio follow-up of GRBs using several-hour integrations to capture the early afterglow evolution and to track the scintillation over a broad frequency range. | - |
dc.description.statementofresponsibility | G. E. Anderson, T. D. Russell, H. M. Fausey, A. J. van der Horst, P. J. Hancock, A. Bahramian, M. E. Bell, J. C. A. Miller-Jones, G. Rowell, M. W. Sammons, R. A. M. J. Wijers, T. J. Galvin, A. J. Goodwin, R. Konno, A. Rowlinson, S. D. Ryder, F. Schussler, S. J. Wagner, and S. J. Zhu | - |
dc.language.iso | en | - |
dc.publisher | Oxford University Press (OUP) | - |
dc.rights | © 2023 The Author(s) | - |
dc.source.uri | http://dx.doi.org/10.1093/mnras/stad1635 | - |
dc.subject | gamma-ray bursts; individual; GRB 210702A; radio continuum; transients | - |
dc.title | Rapid radio brightening of GRB 210702A | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1093/mnras/stad1635 | - |
dc.relation.grant | http://purl.org/au-research/grants/arc/DE180100346 | - |
dc.relation.grant | http://purl.org/au-research/grants/arc/DP200102471 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
Appears in Collections: | Physics publications |
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