Does a long-lived remnant neutron star exist after short gamma-ray burst GRB 160821B?

Wu, G.; Yu, Yun-Wei; Zhu, Jin-Ping

doi:10.1051/0004-6361/202141325

Cited by 12 publications

(9 citation statements)

References 105 publications

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“…When the wind collides with the supernova ejecta, a termination shock can be driven and propagate into the wind. As usual, we termed the shocked wind region as a pulsar wind nebula (PWN), which can in principle contribute to a significant non-thermal emission after the supernova ejecta gradually becomes transparent (Kotera et al 2013;Yu et al 2019;Wu et al 2021). Then, in this section, we try to refit the observational data of SN 2006aj by invoking such a non-thermal PWN emission.…”

Section: Possible Non-thermal Pwn Emissionmentioning

confidence: 98%

The effects of a magnetar engine on the gamma-ray burst-associated supernovae: Application to double-peaked SN 2006aj

Zhang,

Yu,

Liu

2022

Preprint

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A millisecond magnetar engine has been widely suggested to exist in gamma-ray burst (GRB) phenomena, in view of its substantial influences on the GRB afterglow emission. In this paper, we investigate the effects of the magnetar engine on the supernova (SN) emission which is associated with long GRBs and, specifically, confront the model with the observational data of SN 2006aj/GRB 060218. SN 2006aj is featured by its remarkable double-peaked ultraviolet-optical (UV-opt) light curves. By fitting these light curves, we demonstrate that the first peak can be well accounted for by the breakout emission of the shock driven by the magnetar wind, while the primary supernova emission is also partly powered by the energy injection from the magnetar. The magnetic field strength of the magnetar is constrained to be ∼ 10 15 G, which is in good agreement with the common results inferred from the afterglow emission of long GRBs. In more detail, it is further suggested that the UV excess in the late emission of the supernova could also be due to the leakage of the non-thermal emission of the pulsar wind nebula (PWN), if some special conditions can be satisfied. The consistency between the model and the SN 2006aj observation indicates that the magnetar engine is likely to be ubiquitous in the GRB phenomena and even further intensify their connection with the phenomena of superluminous supernovae.

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Section: Possible Non-thermal Pwn Emissionmentioning

confidence: 98%

The effects of a magnetar engine on the gamma-ray burst-associated supernovae: Application to double-peaked SN 2006aj

Zhang,

Yu,

Liu

2022

Preprint

Self Cite

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show abstract

“…When the wind collides with the supernova ejecta, a termination shock can be driven and propagate into the wind. As usual, we termed the shocked wind region as a PWN, which can in principle contribute to a significant nonthermal emission after the supernova ejecta gradually becomes transparent (Kotera et al 2013;Yu et al 2019;Wu et al 2021). Then, in this section, we try to refit the observational data of SN 2006aj by invoking such a nonthermal PWN emission.…”

Section: Possible Nonthermal Pwn Emissionmentioning

confidence: 97%

The Effects of a Magnetar Engine on the Gamma-Ray Burst-associated Supernovae: Application to Double-peaked SN 2006aj

Zhen-Dong

Liu

2022

ApJ

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A millisecond magnetar engine has been widely suggested to exist in gamma-ray burst (GRB) phenomena, in view of its substantial influences on the GRB afterglow emission. In this paper, we investigate the effects of the magnetar engine on the supernova (SN) emission, which is associated with long GRBs and, specifically, confront the model with the observational data of SN 2006aj/GRB 060218. SN 2006aj is featured by its remarkable double-peaked ultraviolet-optical (UV-opt) light curves. By fitting these light curves, we demonstrate that the first peak can be well accounted for by the breakout emission of the shock driven by the magnetar wind, while the primary supernova emission is also partly powered by the energy injection from the magnetar. The magnetic field strength of the magnetar is constrained to be ∼1015 G, which is in good agreement with the common results inferred from the afterglow emission of long GRBs. In more detail, it is further suggested that the UV excess in the late emission of the supernova could also be due to the leakage of the nonthermal emission of the pulsar wind nebula, if some ad hoc conditions can be satisfied. The consistency between the model and the SN 2006aj observation indicates that the magnetar engine is likely to be ubiquitous in the GRB phenomena and even further intensify their connection with the phenomena of superluminous supernovae.

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“…8, give a stringent constraint on the property of the remnant NS, which indicates the complexity of the early evolution of such newborn NSs. In addition, the interaction between the NS wind and merger ejecta can further contribute to a non-thermal emission component, which is detectable when the merger ejecta becomes transparent [90,91].…”

Section: Kilonova/mergernovamentioning

confidence: 99%

Gamma-Ray Bursts

Yu¹,

He²,

Wang³

et al. 2022

Preprint

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Gamma-ray bursts (GRBs) are short and intense bursts of ∼100 keV−1MeV photons, usually followed by long-lasting decaying afterglow emission in a wide range of electromagnetic wavelengths from radio to Xray and, sometimes, even to GeV gamma-rays. These emissions are believed to originate from a relativistic jet, which is driven due to the collapse of special massive stars and the mergers of compact binaries (i.e., double neutron stars or a neutron star and a black hole). This chapter first briefly introduces the basic observational facts of the GRB phenomena, including the prompt emission, afterglow emission, and host galaxies. Secondly, a general theoretical understanding of the GRB phenomena is described based on a relativistic jet's overall dynamical evolution, including the acceleration, propagation, internal dissipation, and deceleration phases. Here a long-lasting central engine of the GRBs can substantially influence the dynamical evolution of the jet. In addition, a supernova/kilonova emission can appear in the optical afterglow of some nearby GRBs, which can provide an important probe to the

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Does a long-lived remnant neutron star exist after short gamma-ray burst GRB 160821B?

Cited by 12 publications

References 105 publications

The effects of a magnetar engine on the gamma-ray burst-associated supernovae: Application to double-peaked SN 2006aj

The effects of a magnetar engine on the gamma-ray burst-associated supernovae: Application to double-peaked SN 2006aj

The Effects of a Magnetar Engine on the Gamma-Ray Burst-associated Supernovae: Application to Double-peaked SN 2006aj

Gamma-Ray Bursts

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