Comparing the size evolution of GRB 221009A with afterglow models

Abstract

We present very long baseline interferometry (VLBI) observations of GRB221009A obtained with the global-VLBI network at 5 GHz between 231 and 750 days after the burst. The quality of our observations allowed us to measure the sub-milliarcsecond full-width at half maximum of the source surface brightness distribution with a one-sigma equivalent error of 13% and 30% at 231 and 391 days post-burst, respectively. By fitting the temporal evolution of these new size measurements alongside those previously published in the literature at 5 and 8 GHz with a single power law ∝ t^a, we find a slope of a = 0.52^+0.14_−0.12. Using the public code VegasAfterglow, we model the 5 GHz size evolution considering the afterglow emission of the forward shock produced by a jet decelerating in either a homogeneous interstellar medium (ISM) or into a surrounding medium with a wind-like density profile. The model constrains the collimation-corrected Sedov ratio, that is, the ratio of the jet kinetic energy Ejet to the density of the surrounding medium (n in the ISM scenario, or A_⋆ in the wind scenario), in the range log[(Ejet/n) erg⁻¹ cm⁻³] = 54.2^+0.4_−0.5 for the ISM scenario and log[(Ejet/A_⋆) erg⁻¹] = 51.7^+0.4_−0.2 for the wind scenario. Among the works in the literature that fit the light curves and spectra of GRB221009A based on the standard afterglow model, and which can be reproduced with VegasAfterglow, none has best-fitting parameters that are compatible with these constraints within 2σ. Moreover, we show that their predicted size evolution is not compatible with the observed one. Our results highlight the importance of size measurements of GRB afterglows as an independent probe of their dynamics, structure, and emission mechanisms.

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BibTeX RIS

BibTeX

@misc{giarratana2026comparing,
  title = {{Comparing the size evolution of GRB 221009A with afterglow models}},
  author = {S. Giarratana and O. S. Salafia and B. Marcote and Z. Paragi and M. Giroletti and G. Ghirlanda and L. Nava and A. van der Horst and J. K. Leung and L. Rhodes and P. G. Edwards and M. Pérez-Torres and J. Yang},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.02988},
  eprint = {2610.02988},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.02988},
  note = {CC BY-NC-ND 4.0},
}

RIS

TY  - UNPB
TI  - Comparing the size evolution of GRB 221009A with afterglow models
AU  - S. Giarratana
AU  - O. S. Salafia
AU  - B. Marcote
AU  - Z. Paragi
AU  - M. Giroletti
AU  - G. Ghirlanda
AU  - L. Nava
AU  - A. van der Horst
AU  - J. K. Leung
AU  - L. Rhodes
AU  - P. G. Edwards
AU  - M. Pérez-Torres
AU  - J. Yang
PY  - 2026
DA  - 2026/10/02
PB  - arXiv
DO  - 10.48550/arxiv.2610.02988
UR  - https://arxiv.org/abs/2610.02988
AB  - We present very long baseline interferometry (VLBI) observations of GRB221009A obtained with the global-VLBI network at 5 GHz between 231 and 750 days after the burst. The quality of our observations allowed us to measure the sub-milliarcsecond full-width at half maximum of the source surface brightness distribution with a one-sigma equivalent error of 13% and 30% at 231 and 391 days post-burst, respectively. By fitting the temporal evolution of these new size measurements alongside those previously published in the literature at 5 and 8 GHz with a single power law ∝ t^a, we find a slope of a = 0.52^+0.14_−0.12. Using the public code VegasAfterglow, we model the 5 GHz size evolution considering the afterglow emission of the forward shock produced by a jet decelerating in either a homogeneous interstellar medium (ISM) or into a surrounding medium with a wind-like density profile. The model constrains the collimation-corrected Sedov ratio, that is, the ratio of the jet kinetic energy E_jet to the density of the surrounding medium (n in the ISM scenario, or A_⋆ in the wind scenario), in the range log[(E_jet/n) erg^−1 cm^−3] = 54.2^+0.4_−0.5 for the ISM scenario and log[(E_jet/A_⋆) erg^−1] = 51.7^+0.4_−0.2 for the wind scenario. Among the works in the literature that fit the light curves and spectra of GRB221009A based on the standard afterglow model, and which can be reproduced with VegasAfterglow, none has best-fitting parameters that are compatible with these constraints within 2σ. Moreover, we show that their predicted size evolution is not compatible with the observed one. Our results highlight the importance of size measurements of GRB afterglows as an independent probe of their dynamics, structure, and emission mechanisms.
ER  -

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