Synchrotron self-compton emission in the two-component jet model for gamma-ray bursts

Sato, Yuri; Obayashi, Kaori; Zhang, B. Theodre; Tanaka, Shuta J.; Murase, Kohta; Ohira, Yutaka; Yamazaki, Ryo

doi:10.1016/j.jheap.2022.12.004

Cited by 11 publications

(8 citation statements)

References 82 publications

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“…According to the two-component model, during the early phase, both components (narrow and wide) of the jet have almost equal velocities. This negligible difference in the velocities helps to discard the possibility of the contribution from the external inverse Compton during the early phase (Sato et al 2022). Therefore, the SSC emission mechanism is expected to explain the early VHE emission in, e.g., GRB 190114C and GRB 190829A (MAGIC Collaboration et al 2019b;HESS Collaboration et al 2021).…”

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

“…The high-luminosity GRBs are typically observed on-axis with narrow viewing; on the other hand, low-luminosity bursts are typically observed offaxis with wide viewing angles. Recently, some authors (Rhodes et al 2022;Sato et al 2022) used two different jet components (narrow and wide) to explain the origin of the observed properties of high-and low-luminosity VHE detected GRBs. According to this model, the early broadband emission of high-luminosity GRBs are explained using a narrow jet component with typical opening angle θ < 0°.…”

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

“…86. On the other hand, low-luminosity GRBs are explained using a wide jet component with typical opening angle θ > 6° (Sato et al 2022). Sato et al (2022) performed broadband modeling of the nearby and low-luminosity GRB 190829A using a two-component jet model and noted that the prompt and afterglow emissions could not be described by a narrow jet component.…”

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

“…On the other hand, low-luminosity GRBs are explained using a wide jet component with typical opening angle θ > 6° (Sato et al 2022). Sato et al (2022) performed broadband modeling of the nearby and low-luminosity GRB 190829A using a two-component jet model and noted that the prompt and afterglow emissions could not be described by a narrow jet component. The observed low/intermediate-luminosity nature of GRB 190829A is explained by assuming that the viewing angle is greater than the opening angle of its narrow jet component (off-axis observations).…”

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

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Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror

Gupta

Jelínek

et al. 2023

ApJ

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We present a detailed prompt emission and early optical afterglow analysis of the two very-high-energy (VHE) detected bursts GRB 201015A and GRB 201216C, and their comparison with a subset of similar bursts. Time-resolved spectral analysis of multistructured GRB 201216C using the Bayesian binning algorithm revealed that during the entire duration of the burst, the low-energy spectral index (α pt) remained below the limit of the synchrotron line of death. However, statistically some of the bins supported the additional thermal component. Additionally, the evolution of spectral parameters showed that both the peak energy (E p) and α pt tracked the flux. These results were further strengthened using the values of the physical parameters obtained by synchrotron modeling of the data. Our earliest optical observations of both bursts using the F/Photometric Robotic Atmospheric Monitor Observatorio del Roque de los Muchachos and Burst Observer and Optical Transient Exploring System robotic telescopes displayed a smooth bump in their early optical light curves, consistent with the onset of the afterglow due to synchrotron emission from an external forward shock. Using the observed optical peak, we constrained the initial bulk Lorentz factors of GRB 201015A and GRB 201216C to Γ0 = 204 and Γ0 = 310, respectively. The present early optical observations are the earliest known observations constraining outflow parameters and our analysis indicate that VHE detected bursts could have a diverse range of observed luminosity within the detectable redshift range of present VHE facilities.

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Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

Section: Possible Origin Of Vhe Emission From High-and Lowluminosity ...mentioning

confidence: 99%

See 2 more Smart Citations

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror

Gupta

Jelínek

et al. 2023

ApJ

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“…It is generally believed that the VHE afterglows of GRBs are attributed to the synchrotron, synchrotron self-Compton (SSC), and/or external inverse-Compton (EIC) radiations of the electrons accelerated in the jets (e.g., Dermer et al 2000;Sari & Esin 2001;Zhang & Mészáros 2001;MAGIC Collaboration et al 2019b;Acciari et al 2021;H.E.S.S. Collaboration et al 2021;Zhang et al 2021b;Sato et al 2023). The broadband spectral energy distribution (SED) in the optical, X-ray, and sub-TeV gamma-ray bands of GRB 190114C can be roughly modeled with the synchrotron radiations and SSC process of the ultrarelativistic electrons in the jet (e.g., Wang et al 2019;Huang et al 2020;Zhang et al 2020;Joshi & Razzaque 2021;Yamasaki & Piran 2022).…”

Section: Introductionmentioning

confidence: 99%

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Zhang

Ren

Wang

et al. 2023

ApJ

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Gamma-ray bursts (GRBs) 201015A and 201216C are valuable cases where very-high-energy (VHE) gamma-ray afterglows have been detected. By analyzing their prompt emission data, we find that GRB 201216C is an extremely energetic, long GRB with a hard gamma-ray spectrum, while GRB 201015A is a relative subenergetic, soft-spectrum GRB. Attributing their radio–optical–X-ray afterglows to the synchrotron radiation of the relativistic electrons accelerated in their jets, we fit their afterglow lightcurves with the standard external shock model and infer their VHE afterglows from the synchrotron self-Compton scattering process of the electrons. It is found that the jet of GRB 201015A is midrelativistic (Γ0 = 44), surrounded by a very dense medium (n = 1202 cm−3), and the jet of GRB 201216C is ultrarelativistic (Γ0 = 331), surrounded by a moderate dense medium (n = 5 cm−3). The inferred peak luminosity of the VHE gamma-ray afterglows of GRB 201216C is approximately 10−9 erg cm−2 s−1 at 57–600 s after the GRB trigger, making it detectable with the MAGIC telescopes at a high confidence level, even though the GRB is at a redshift of 1.1. Comparing their intrinsic VHE gamma-ray lightcurves and spectral energy distributions with GRBs 180720B, 190114C, and 190829A, we show that their intrinsic peak luminosity of VHE gamma-ray afterglows at 104 s after the GRB trigger is variable from 1045 to 5 × 1048 erg s−1, and their kinetic energy, initial Lorentz factor, and medium density are diverse among bursts.

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Early photometric and spectroscopic observations of the extraordinarily bright INTEGRAL-detected GRB 221009A

Sánchez-Ramírez,

Lang,

Pozanenko

et al. 2024

A&A

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initially detected as an X-ray transient by was later revealed to have triggered the satellite about an hour earlier, marking it as a post-peak observation of the event's emission. This GRB distinguished itself as the brightest ever recorded, presenting an unparalleled opportunity to probe the complexities of GRB physics. The unprecedented brightness, however, challenged observation efforts, as it led to the saturation of several high-energy instruments. Our study seeks to investigate the nature of the and elucidate the environmental conditions conducive to these exceptionally powerful bursts. Moreover, we aim to understand the fundamental physics illuminated by the detection of teraelectronvolt (TeV) photons emitted by grb. We conducted detailed analyses of early photometric and spectroscopic observations that span from the trigger through to the initial days following the prompt emission phase in order to characterize afterglow, and we complemented these analyses with a comparative study. Our findings from analyzing data confirm as the most energetic event observed to date. Early optical observations during the prompt phase negate the presence of bright optical emissions with internal or external shock origins. Spectroscopic analyses enabled us to measure distance and line-of-sight properties. The afterglow's temporal and spectral analysis suggests prolonged activity of the central engine and a transition in the circumburst medium's density. Finally, we discuss the implications for fundamental physics of detecting photons as energetic as 18 TeV from grb. Early optical observations have proven invaluable for distinguishing between the potential origins of optical emissions in underscoring their utility in GRB physics studies. However, the rarity of such data underscores the need for dedicated telescopes capable of synchronous multiwavelength observations. Additionally, our analysis suggests that the host galaxies of TeV GRBs share commonalities with those of long and short GRBs. Expanding the sample of TeV GRBs could further solidify these findings.

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Synchrotron self-compton emission in the two-component jet model for gamma-ray bursts

Cited by 11 publications

References 82 publications

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Early photometric and spectroscopic observations of the extraordinarily bright INTEGRAL-detected GRB 221009A

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