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GRB 241030A: A bright afterglow challenging forward shock emission

J. G. DucoinAix-Marseille Univ., CNRS/IN2P3, Ctr. de Physique des Particules de Marseille, IPhUClément PellouinThe Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv UniversityV. AivazyanE. Kharadze Georgian National Astrophysical ObservatoryDalya AklCenter for Astrophysics and Space Science (CASS), New York University Abu DhabiF Javier AlvarezInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoCristina AndradeSchool of Physics and Astronomy, University of MinnesotaCamila Angulo-ValdezInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoS. AntierUniversité de la Côte d’AzurJ. L. AtteiaUniversité Toulouse III - Paul SabatierS. BasaAix Marseille Univ., CNRS, CNES, LAMR. L. BecerraInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoZ. BenkhaldounOukaimeden Observatory and High Energy Physics, Astrophysics and Geoscience Laboratory, FSSM, Cadi Ayyad UniversityC. MeeganPolitecnico di MilanoA. A. BreeveldMullard Space Science Laboratory – University College LondonEmma de BruinSchool of Physics and Astronomy, University of MinnesotaEric BurnsDepartment of Physics & Astronomy, Louisiana State UniversityN. ButlerSchool of Earth and Space Exploration, Arizona State UniversityM. W. CoughlinSchool of Physics and Astronomy, University of MinnesotaF. DaigneInstitut d'Astrophysique de ParisT. DietrichMax Planck Institute for Gravitational Physics (Albert Einstein Institute)Damien DornicAix-Marseille Univ., CNRS/IN2P3, Ctr. de Physique des Particules de Marseille, IPhUC. DouzetIJCLab, Univ Paris-Saclay, CNRS/IN2P3T. du LazCahill Center for Astrophysics, California Institute of TechnologyPierre-Alexandre DuverneUniversité Paris CitéH.-B. EggensteinKNC, Volkssternwarte PaderbornE. G. ElhosseinyNational Research Institute of Astronomy and Geophysics (NRIAG)Ali EsamdinUniversity of Chinese Academy of SciencesN. GehrelsSchool of Physics and Astronomy, University of LeicesterJ. F. Agüí FernándezObservatorio de Calar AltoM. FerroOsservatorio Astronomico di BreraFrancis FortinInstitut de Recherche en Astrophysique et PlanétologieM FreebergKNC, AAVSO, Hidden Valley Observatory(HVO)Leonardo García-GarcíaInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoRamandeep GillInstituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de MéxicoNoémie GlobusInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoN. GuessoumAmerican University of Sharjah, Physics DepartmentGamal M. HamedNational Research Institute of Astronomy and Geophysics (NRIAG)Patrice HelloUniversité Paris-SaclayA H AirascaUniversity of TrentoD. F. HuPurple Mountain Observatory, Chinese Academy of SciencesT. Hussenot-DesenongesIJCLab, Univ Paris-Saclay, CNRS/IN2P3R. InasaridzeSamtskhe-Javakheti State UniversityA. IskandarUniversity of Chinese Academy of SciencesS. Q. JiangNational Astronomical Observatories, Chinese Academy of SciencesChichuan JinNetherlands Institute for Radio AstronomyAziz Ettahar KaeouachOukaimeden Observatory and High Energy Physics, Astrophysics and Geoscience Laboratory, FSSM, Cadi Ayyad UniversityС. КарповFZU – Institute of Physics of the Czech Academy of SciencesN. J. KlinglerCenter for Space Sciences and Technology, University of MarylandA. KlotzUniversité Fédérale de Toulouse Midi-PyrénéesN. KochiashviliE. Kharadze Georgian National Astrophysical ObservatoryHauke KöhnInstitute of Physics and Astronomy, Theoretical Astrophysics, University PotsdamR. KneipKNCT. KvernadzeE. Kharadze Georgian National Astrophysical ObservatoryA. Le CallochSchool of Physics and Astronomy, University of MinnesotaWilliam H. LeeInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoA. LekicKNC, Institut Polytechnique des Sciences Avancées: Ivry-sur-SeineY. F. LiangSchool of Astronomy and Space Sciences, University of Science and Technology of ChinaC. LimontaUniversité de la Côte d’AzurJ. LiuPhysics Department, Tsinghua UniversityK. LópezInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoDiego López-CámaraInstituto de Ciencias Nucleares, Universidad Nacional Autónoma de MéxicoRaouf H. MabroukNational Research Institute of Astronomy and Geophysics (NRIAG)F. MagnaniAix-Marseille Univ., CNRS/IN2P3, Ctr. de Physique des Particules de Marseille, IPhUJ. MaoYunnan Observatories, Chinese Academy of SciencesM. MašekFZU – Institute of Physics of the Czech Academy of SciencesEnrique Moreno MéndezFacultad de Ciencias, Universidad Nacional Autónoma de MéxicoB. MihovInstitute of Astronomy and NAO, Bulgarian Academy of SciencesM. MolhamNational Research Institute of Astronomy and Geophysics (NRIAG)K. NoysenaNational Astronomical Research Institute of Thailand (NARIT)Mohammad OdehKNC, International Astronomical CenterN. OmodeiW.W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford UniversityH. PengPhysics Department, Tsinghua UniversityMargarita PereyraInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoM. PillasSorbonne UniversitéR. PilleraIstituto Nazionale de Fisica Nucleare (INFN) – Sezione di BariT. PradierUniversité de Strasbourg, CNRS, IPHC UMR 7178Y RajabovUlugh Beg Astronomical Institute, Uzbekistan Academy of SciencesN.A. RakotondrainibeAix Marseille Univ., CNRS, CNES, LAMBenjamin SchneiderAix Marseille Univ., CNRS, CNES, LAMM. SerrauKNC, Société Astronomique de France, Observatoire de DaubanL. Slavcheva-MihovaInstitute of Astronomy and NAO, Bulgarian Academy of SciencesOleksii SokoliukAstronomical ObservatoryH. SunNational Astronomical ObservatoriesA. TakeyNational Research Institute of Astronomy and Geophysics (NRIAG)M. TanasanNational Astronomical Research Institute of Thailand (NARIT)K. S. TinyanontNational Astronomical Research Institute of Thailand (NARIT)D. TurpinUniversité Paris CitéA. de Ugarte PostigoAix Marseille Univ., CNRS, CNES, LAMBaofan WangUniversity of Chinese Academy of SciencesL.T. WangPhysics Department, Tsinghua UniversityXiaofeng WangPhysics Department, Tsinghua UniversityZ. M. WangInstitute for Frontier in Astronomy and Astrophysics, Beijing Normal UniversityA. M. WatsonInstituto de Astronomía, Universidad Nacional Autónoma de MéxicoHongzhou WuDepartment of Astronomy, School of Physics, Huazhong University of Science and TechnologyQinyu WuSchool of Astronomy and Space Science, University of Chinese Academy of SciencesJ Q XuKey Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of SciencesY. S. YanPhysics Department, Tsinghua UniversityHaonan YangNational Astronomical Observatories, Chinese Academy of SciencesW. YuanNational Astronomical ObservatoriesHongyun ZhaoKey Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences

2026en

ABI

Annotatsiya

Context. Gamma-ray burst GRB 241030A ( z = 1.411) exhibited a particularly bright afterglow (similar to the ‘BOAT’, GRB 221009A), detected across gamma-ray, X-ray, UV, and optical bands. The extensive, multi-wavelength observations of this remarkable event provide a valuable opportunity to advance our understanding of GRB afterglow physics. Aims. We aim to constrain the physical properties of the jet, its microphysics, and the characteristics of the circumburst environment in the context of forward-shock emission. Methods. We compiled multi-wavelength observations spanning from a minute to a week after the prompt emission, processing the data through a unified photometry pipeline. Leveraging this comprehensive dataset, we analysed the observations both analytically and using Bayesian inference with two independent models. Our models assume that the afterglow emission arises from the strong forward shock of a laterally structured jet, with possible contributions from synchrotron self-Compton (SSC) scatterings. Results. We find that our models do reproduce the afterglow observations accurately, from the X-rays to the optical, favouring a jet propagating into a constant-density interstellar medium, with a viewing angle within the jet core. However, both analyses – with and without the inclusion of SSC scatterings – require parameter values that are extreme compared to expectations from standard theory. In particular, our results imply extremely energetic jets despite regular prompt energy, leading to a very inefficient prompt emission. Furthermore, the jets are particularly inefficient at accelerating particles, with low ϵ e and ϵ B , leading to significant SSC emission. Finally, our analyses indicate that the jets have large opening angles and propagate in high-density media. Conclusions. If the afterglow is indeed powered by radiation emitted behind a strong forward shock, our results place GRB 241030A within a sub-class of GRBs characterised by extreme kinetic energies, large jet opening angles, and very low prompt emission efficiencies, below 10 −3 , with strong SSC radiation. These predictions are difficult to reconcile with typical expectations from other GRBs. We therefore suggest that the afterglow of GRB 241030A is not solely powered by forward shock emission, and we discuss other options such as a long-lasting reverse-shock contribution.

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DOI: 10.1051/0004-6361/202558838

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