The BOAT GRB 221009A: A Poynting-flux-dominated narrow jet surrounded by a matter-dominated structured jet wing

Zhang, Bing; Wang, Xiang-Yu; Zheng, Jian-He

doi:10.1016/j.jheap.2024.01.002

Cited by 6 publications

(7 citation statements)

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“…The early sharp break in the TeV band is consistent with a jet break from a top-hat jet (LHAASO Collaboration 2023), while the later shallow break could be due to the change of the angular profile dE/dΩ ∝ θ − a of a structured jet (Gill & Granot 2023;O'Connor et al 2023). This complex behavior suggests a jet composed of an inner, narrow top-hat core component and an outer, wide wing component with an angular structure, which can be described by (Zhang et al 2024)…”

Section: The Setup Of a Two-component Jet Modelmentioning

confidence: 68%

“…The narrow jet core could be a Poynting-flux-dominated jet (Dai et al 2023;Yang et al 2023), and the wide wing could be matter-dominated, as argued in Zhang et al (2024).…”

Section: Jmentioning

confidence: 94%

“…For a wing with an angular profile dE/dΩ ∝ θ − a , the light curve of the synchrotron emission from the forward shock is given by (Beniamini et al 2022;Zhang et al 2024)…”

Section: The Optical-to-tev Afterglowsmentioning

confidence: 99%

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A Narrow Uniform Core with a Wide Structured Wing: Modeling the TeV and Multiwavelength Afterglows of GRB 221009A

Zheng,

Wang,

Liu

et al. 2024

ApJ

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The TeV afterglow of the BOAT GRB 221009A was interpreted as arising from a narrow jet, while the radio-to-X-ray afterglows were interpreted as arising from a wide structured jet. However, there is no model explaining the TeV and lower-energy multiwavelength afterglows simultaneously. We here investigate a two-component jet model, including a narrow uniform core with a wide structured wing, to explain both the multiwavelength afterglows that last up to 100 days. We find that to explain the early TeV afterglow with the inverse-Compton process, we need a circumburst density higher than ≳0.1 cm−3, while the radio afterglow and the H.E.S.S. upper limit combine to constrain the density to be lower at larger radii. Thus, a decreasing density profile with radius is favored. Considering that the rising TeV light curve during the afterglow onset favors a constant-density medium, we invoke a stratified density profile, including a constant-density profile at small radii and a wind density profile at large radii. We find that the two-component jet model with such a stratified density profile can explain the TeV, X-ray, and optical afterglows of GRB 221009A, although the radio fluxes exceed the observed ones by a factor of 2 at later epochs. The discrepancy in the radio afterglow could be resolved by invoking some nonstandard assumption about the microphysics of afterglow shocks. The total kinetic energy of the two components in our model is ≲1052 erg, significantly smaller than that in the single structured jet models.

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Section: The Setup Of a Two-component Jet Modelmentioning

confidence: 68%

“…The narrow jet core could be a Poynting-flux-dominated jet (Dai et al 2023;Yang et al 2023), and the wide wing could be matter-dominated, as argued in Zhang et al (2024).…”

Section: Jmentioning

confidence: 94%

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A Narrow Uniform Core with a Wide Structured Wing: Modeling the TeV and Multiwavelength Afterglows of GRB 221009A

Zheng,

Wang,

Liu

et al. 2024

ApJ

Self Cite

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“…Instead, a large energy dissipation radius of 10 15 -10 16 cm is natural for a Poynting-flux-dominated GRB outflow (e.g., Fan et al 2005;Zhang & Yan 2011;Kumar & Zhang 2015). Indeed, recently, Zhang et al (2024) suggested that the ejecta of GRB 221009A was composed of a narrow (∼0°.6 half opening angle) Poynting-flux-dominated outflow composition and a broader matter-dominated jet wing. In the future, a successful detection of the UHECR outburst from GRB 221009A will not only directly establish the GRB-UHECR connection, but also provide us a valuable chance to measure or stringently constrain the IGMF and the GMF, and key parameters of the GRB physics, such as the energy dissipation radius, the bulk Lorentz factor and the baryon loading factor of the jet, and further reveal the radiation mechanism and the central engine of the GRB.…”

Section: Results and Prospectsmentioning

confidence: 99%

A Detectable Ultra-high-energy Cosmic-Ray Outburst from GRB 221009A

He,

Zhang,

Fan

2024

ApJ

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Gamma-ray bursts (GRBs) have been proposed as one of the promising sources of ultra-high-energy cosmic rays (UHECRs), but observational evidence is still lacking. The nearby brightest of all time GRB 221009A, a once in 1000 yr event, is able to accelerate protons to ∼103 EeV, and then generate extremly energetic neutrons via the photomeson production interaction. Protons arriving at the Milky Way are dominated by neutron-decay-induced protons. The intergalactic magnetic fields would not yield a sizable delay of the ≥10 EeV cosmic rays if its strength is ≲10−13 G, while Galactic magnetic fields would cause a significant time delay. We predict that a UHECR burst from GRB 221009A would be detectable by the Pierre Auger Observatory and the TA×4, within ∼10 yr. The detection of such a UHECR outburst will provide the direct evidence for UHECR acceleration in GRBs.

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“…In this structured jet model, the narrow jet core with ultrarelativistic Lorentz factor should be surrounded by a wider jet with a lower Lorentz factor, leading to complicated temporal and spectral features (e.g., Panaitescu et al 2006;Racusin et al 2008). A joint analysis of the early and late afterglow of GRB 221009A could further deepen our understanding of GRB and jet physics (e.g., Gill & Granot 2023;O'Connor et al 2023;Ren et al 2023;Sato et al 2023;Zhang et al 2024).…”

Section: Discussionmentioning

confidence: 99%

Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands

Zheng,

Zhang,

Xiong

et al. 2024

ApJL

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The early afterglow of a gamma-ray burst (GRB) can provide critical information on the jet and progenitor of the GRB. The extreme brightness of GRB 221009A allows us to probe its early afterglow in unprecedented detail. In this Letter, we report comprehensive observation results of the early afterglow of GRB 221009A (from T 0+660 s to T 0+1860 s, where T 0 is the Insight-HXMT/HE trigger time) in X-ray/gamma-ray energy band (from 20 keV to 20 MeV) by Insight-HXMT High Energy X-ray Telescope, GECAM-C, and Fermi/Gamma-ray Burst Monitor. We find that the spectrum of the early afterglow in 20 keV–20 MeV can be well described by a cutoff power law with an extra power law that dominates the low- and high-energy bands, respectively. The cutoff power law E peak is ∼30 keV, and the power-law photon index is ∼1.8 throughout the early afterglow phase. By fitting the light curves in different energy bands, we find that a significant achromatic break (from keV to TeV) is required at T 0 + 1246 − 26 + 27 s (i.e., 1021 s since the afterglow starting time T AG = T 0+225 s), providing compelling evidence of a jet break. Interestingly, both the pre-break and post-break decay slopes vary with energy, and these two slopes become closer in the lower energy band, making the break less identifiable. Intriguingly, the spectrum of the early afterglow experienced a slight hardening before the break and a softening after the break. These results provide new insights into the physics of this remarkable GRB.

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The BOAT GRB 221009A: A Poynting-flux-dominated narrow jet surrounded by a matter-dominated structured jet wing

Cited by 6 publications

References 75 publications

A Narrow Uniform Core with a Wide Structured Wing: Modeling the TeV and Multiwavelength Afterglows of GRB 221009A

A Narrow Uniform Core with a Wide Structured Wing: Modeling the TeV and Multiwavelength Afterglows of GRB 221009A

A Detectable Ultra-high-energy Cosmic-Ray Outburst from GRB 221009A

Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands

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