Axion dark matter from first-order phase transition, and very high energy photons from GRB 221009A

Nakagawa, Shota; Takahashi, Fuminobu; Yamada, Masaki; Yin, Wen

doi:10.1016/j.physletb.2023.137824

Cited by 33 publications

(19 citation statements)

References 75 publications

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“…This new discovery opened the observation window of γ-ray emissions of GRBs in the TeV band and confirmed the new radiation mechanism expected by the model, named the IC process (Mészáros & Rees 1994;Dermer et al 2000;Sari & Esin 2001;Zhang & Mészáros 2001). Those discoveries shined a new light on the central engine and radiation mechanism and probed new physics such as LIV and Dark Matter (DM) (Amelino-Camelia et al 1998;Nakagawa et al 2023;González et al 2023). It is unfortunate that the γ-ray emissions at TeV energy were only observed at the afterglow phase of LGRBs.…”

Section: Introductionsupporting

confidence: 54%

Prospects for detection rate of very-high-energy γ-ray emissions from short γ-ray bursts with the HADAR experiment

Chen¹,

Hu²,

Su³

et al. 2023

Preprint

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The observation of short gamma ray bursts (SGRBs) in the TeV energy range plays an important role in understanding the radiation mechanism and probing new areas of physics such as Lorentz invariance violation. However, no SGRB has been observed in this energy range due to the short duration of SGRBs and the weakness of current experiments. New experiments with new technology are required to detect sub-TeV SGRBs. In this work, we observe the very high energy (VHE) γray emissions from SGRBs and calculate the annual detection rate with the High Altitude Detection of Astronomical Radiation HADAR (HADAR) experiment. First, a set of pseudo-SGRB samples is generated and checked using the observations of Fermi-GBM, Fermi-LAT, and SWIFT measurements. The annual detection rate is calculated from these SGRB samples based on the performance of the HADAR instrument. As a result, the HADAR experiment can detect 0.5 SGRB per year if the spectral break-off of γ-rays caused by the internal absorption is larger than 100 GeV. For a GRB09010-like GRB in HADAR's view, it should be possible to detect approximately 2000 photons considering the internal absorption. With a time delay assumption due to the Lorentz invariance violation effects, a simulated light curve of GRB090510 has evident energy dependence. We hope that the HADAR experiment can perform the SGRB observations and test our calculations in the future.

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Section: Introductionsupporting

confidence: 54%

Prospects for detection rate of very-high-energy γ-ray emissions from short γ-ray bursts with the HADAR experiment

Chen¹,

Hu²,

Su³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…This is corresponding to the radiation luminosity greater than ∼6.5 × 10 53 erg s −1 at ∼18 TeV. Some possibilities can explain this phenomenon, such as hadronic processes (e.g., synchrotron radiation of protons; Aharonian 2000;Alves et al 2018), Lorentz invariance violation (LIV), and axion-like particles (e.g., Galanti et al 2022;Nakagawa et al 2023;Finke & Razzaque 2023;Li & Ma 2023), or the need for corrections to the EBL field of low-energy photons.…”

Section: Spectral Energy Distributionmentioning

confidence: 97%

The Possibility of Modeling the Very High Energy Afterglow of GRB 221009A in a Wind Environment

Ren

Wang

Zhang

et al. 2023

ApJ

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In this paper, we model the dynamics and radiation physics of the rarity event GRB 221009A afterglow in detail. By introducing a top-hat jet that propagates in an environment dominated by stellar winds, we explain the publicly available observations of afterglow associated with GRB 221009A over the first week. It is predicted that GRB 221009A emits a luminous very high energy afterglow based on the synchrotron self-Compton (SSC) process in our model. We show the broadband spectral energy distribution (SED) analysis results of GRB 221009A and find that the SSC radiation component of GRB 221009A is very bright in the 0.1–10 TeV band. The integrated SED shows that the SSC emission in the TeV band has detection sensitivity significantly higher than that of LHASSO, MAGIC, and CTA. However, since the release of further observations, deviations from the standard wind environment model have gradually shown up in data. For example, the late-time multiband afterglow cannot be consistently explained under the standard wind environment scenario. It may be necessary to consider modeling with a structured jet with complex geometry or a partial revision of the standard model. Furthermore, we find that the inclusion of GeV observations could break the degeneracy between model parameters, highlighting the significance of high-energy observations in determining accurate parameters for GRB afterglows.

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“…) is ΔE/E ∼ 45% for LHAASO-KM2A and ΔE/ E ∼ 60% for LHAASO-WCDA. Our results indicate that even without considering the effect of new physics on the propagation of VHE gamma rays, e.g., photon mixing with axion-like particles (Baktash et al 2022;Galanti et al 2022;Nakagawa et al 2023;Troitsky 2022) and Lorentz invariance violation (Finke & Razzaque 2022;Li & Ma 2022;Zhu & Ma 2022), the detection of ∼18 TeV photons by LHAASO-KM2A can be explained for reasonable EBL models. Another possible explanation for the detection of ∼18 TeV is the intergalactic electromagnetic cascade due to the propagation of UHECRs (Batista 2022;Das & Razzaque 2022;Mirabal 2022).…”

Section: Implications For Lhaaso Detectionmentioning

confidence: 79%

External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A

Zhang

Murase

Ioka

et al. 2023

ApJL

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The detection of the hyper-bright gamma-ray burst (GRB) 221009A enables us to explore the nature of the GRB emission and the origin of very high-energy gamma rays. We analyze the Fermi Large Area Telescope (Fermi-LAT) data of this burst and investigate the GeV–TeV emission in the framework of the external reverse-shock model. We show that the early ∼1–10 GeV emission can be explained by the external inverse-Compton mechanism via upscattering MeV gamma rays by electrons accelerated at the reverse shock, in addition to the synchrotron self-Compton component. The predicted early optical flux could have been brighter than that of the naked-eye GRB 080319B. We also show that proton synchrotron emission from accelerated ultrahigh-energy cosmic rays (UHECRs) is detectable and could potentially explain ≳TeV photons detected by LHAASO or constrain the UHECR acceleration mechanism. Our model suggests that the detection of  ( 10 TeV ) photons with energies up to ∼18 TeV is possible for reasonable models of the extragalactic background light without invoking new physics and predicts anticorrelations between MeV photons and TeV photons, which can be tested with the LHAASO data.

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Axion dark matter from first-order phase transition, and very high energy photons from GRB 221009A

Cited by 33 publications

References 75 publications

Prospects for detection rate of very-high-energy γ-ray emissions from short γ-ray bursts with the HADAR experiment

Prospects for detection rate of very-high-energy γ-ray emissions from short γ-ray bursts with the HADAR experiment

The Possibility of Modeling the Very High Energy Afterglow of GRB 221009A in a Wind Environment

External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A

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