Polarization in Early Optical Afterglows of Gamma-Ray Bursts Driven by Precessing Jets

Huang, Baoquan; Liu, Tong

doi:10.3847/1538-4357/ac752a

Cited by 4 publications

(2 citation statements)

References 72 publications

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“…In this case, the X-ray afterglows are likely to contain several X-ray flares of similar widths in linear scale and similar spectra, and the optical afterglow light curve will show sharp rebrightening signatures (Chen et al 2022). While in the jet precession scenario, it is expected that peculiar polarization features in early optical afterglows (Huang & Liu 2022) and special energy injection signatures in X-ray/optical afterglows (Huang & Liu 2021) will be observed . Lin et al (2022) performed a systemic search among ∼3000 GRBs, and only four GRBs are found to consist of multiple similar emission episodes.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

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Repeating Emission Episodes in Gamma-Ray Bursts: Millilensing or Jet Precession?

Liu

Lei

You

2023

ApJ

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Recently, some gamma-ray bursts (GRBs) whose light curves consist of repeating emission episodes with similar temporal profiles have attracted extensive attention. They are proposed to be candidates of millilensing events, although smoking gun evidence is lacking, since there are no redshift measurements and no angular offset detections for any of these candidates. Here we show that without invoking gravitational lensing, the repeating light-curve properties of these GRBs could also be interpreted under the jet precession model, as long as the detectable period in every precession circle is less than the precession period, and the precession period is close to the jet emission duration. By fitting the gamma-ray light curves of these GRBs, we suggest that the jet precession angle for these bursts should be relatively small (e.g., θ p < 5.°3), and the jet structure for these bursts are more likely Gaussian. The results suggest us to be careful when identifying millilensing GRBs. Multiband afterglow data and especially angular offset detections are essential to provide comprehensive justification for this identification.

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Section: Conclusion and Discussionmentioning

confidence: 99%

“…Our results suggest to us to be careful when identifying millilensing GRBs. Multiband afterglow data and especially angular offset detections are essential to provide comprehensive justification of such an identification (Huang & Liu 2021;Chen et al 2022;Huang & Liu 2022).…”

Section: Introductionmentioning

confidence: 99%

Repeating Emission Episodes in Gamma-Ray Bursts: Millilensing or Jet Precession?

Liu

Lei

You

2023

ApJ

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Prompt GRB polarization from non-axisymmetric jets

Gill,

Granot

2023

Monthly Notices of the Royal Astronomical Society

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Time-resolved linear polarization (Π) measurements of the prompt gamma-ray burst emission can reveal its dominant radiation mechanism. A widely considered mechanism is synchrotron radiation, for which linear polarization can be used to probe the jet’s magnetic-field structure, and in turn its composition. In axisymmetric jet models the polarization angle (PA) can only change by 90○, as Π temporarily vanishes. However, some time-resolved measurements find a continuously changing PA, which requires the flow to be non-axisymmetric in at least one out of its emissivity, bulk Lorentz factor or magnetic field. Here we consider synchrotron emission in non-axisymmetric jets, from an ultrarelativistic thin shell, comprising multiple radially-expanding mini-jets (MJs) or emissivity patches within the global jet, that yield a continuously changing PA. We explore a wide variety of possibilities with emission consisting of a single pulse or multiple overlapping pulses, presenting time- resolved and integrated polarization from different magnetic field configurations and jet angular structures. We find that emission from multiple incoherent MJs/patches reduces the net polarization due to partial cancellation in the Stokes plane. When these contain a large-scale ordered field in the plane transverse to the radial direction, Π always starts near maximal and then declines over the single pulse or shows multiple highly polarized peaks due to multiple pulses. Observing $\Pi \lesssim 40~{{\%}}$ (15%) integrated over one (several) pulse(s) will instead favor a shock-produced small-scale field either ordered in the radial direction or tangled in the plane transverse to it.

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Low-frequency Gravitational-wave Memories from Gamma-Ray Burst Afterglows with Energy Injections

Huang

Liu

Xue

et al. 2023

ApJ

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Ultrarelativistic gamma-ray burst (GRB) jets are strong gravitational-wave (GW) sources with memory-type signals. The plateau (or shallow decay) phases driven by the energy injection may appear in the early X-ray afterglows of GRBs. In this paper, we investigate GW signals as well as X-ray afterglow emissions in the framework of GRB jets with energy injections, and both short- and long-duration GRBs are considered. We find that, regardless of the case, and because of the antibeaming and time delay effects, a rising slope that emerges in the waveform of the GW signal, due to the energy injection, lags far behind the energy ejection, and the typical frequencies of the characteristic amplitudes fall within a low-frequency region of ∼10−4–10−6 Hz; we also consider that the GW memories triggered by the GRB jets with energy injection have previously not been accounted for and that nearby GRBs with strong energy injections may disturb the measurement of the stochastic GW background. Such GW memory detection would provide a direct test for models of energy injection in the scenario of GRB jets.

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Polarization in Early Optical Afterglows of Gamma-Ray Bursts Driven by Precessing Jets

Cited by 4 publications

References 72 publications

Repeating Emission Episodes in Gamma-Ray Bursts: Millilensing or Jet Precession?

Repeating Emission Episodes in Gamma-Ray Bursts: Millilensing or Jet Precession?

Prompt GRB polarization from non-axisymmetric jets

Low-frequency Gravitational-wave Memories from Gamma-Ray Burst Afterglows with Energy Injections

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