Sharp Decay of the Internal Plateau in Gamma-Ray Bursts: The Effect of a Cocoon's Thermal Photons on the Jet Emission

Li, Yu-Fei; Lin, Da-Bin; Ren, Jia; Li, Xiao-Yan; Li, Guo-Peng; Liang, En-Wei

doi:10.3847/1538-4357/ad08bc

Cited by 2 publications

(1 citation statement)

References 77 publications

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“…External plateaus can be explained by emission from the external shock. The second type is an internal plateau, which exhibits a rapid decay at the end of the plateau phase, i.e., Δt/t = 1, which is very different from that of the external-forward shock (Rowlinson et al 2013;Lü et al 2015;Gompertz et al 2020;Li et al 2024). This reveals that the central engine drives the internal plateaus and the abrupt cutoff is attributed to the collapse of an NS in Cases III-IV.…”

Section: Sample Of Sgrbs With An Internal Plateaumentioning

confidence: 93%

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Li,

Chen,

Lin

et al. 2024

ApJ

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The merger of a neutron star (NS)–NS binary can form different productions of compact remnants, among which a supramassive NS (SMNS) can create an internal plateau, and the following steep decay marks the collapse of the SMNS. The proportion of the SMNS and the corresponding collapse time are often used to constrain the NS equation of state (EOS). This paper revisits this topic by considering the effect of an accretion disk on a compact remnant, which is not considered in previous works. Compared with previous works, the collapse-time distribution (peaks ∼100 s) of SMNSs formed from an NS–NS merger is almost unaffected by the initial surface magnetic field (B s,i ) of the NS, but the total energy output of the magnetic dipole radiation from the SMNSs depends on B s,i significantly. Coupling the constraints from the SMNS fraction, we exclude some EOSs and obtain three candidate EOSs, i.e., DD2, ENG, and MPA1. By comparing the distributions of the collapse time and the luminosity of the internal plateau (in the short gamma-ray bursts) for observations obtained based on the three candidate EOSs, it is shown that only the EOS of ENG is favored. Our sample, based on the ENG EOS and a mass distribution motivated by Galactic systems, suggests that approximately 99% of NS–NS mergers collapse to form a black hole (BH) within 107s. This includes scenarios promptly forming a BH (36.5%), an SMNS (60.7%), or a stable NS that transitions into a BH or an SMNS following accretion (2.1%). It also indicates that the remnants for GW170817 and GW190425, and the second object of GW190814, are more likely to be BHs.

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Section: Sample Of Sgrbs With An Internal Plateaumentioning

confidence: 93%

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Li,

Chen,

Lin

et al. 2024

ApJ

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The Effect of Anisotropic Energy Injection on the Ejecta Emission

Li,

Lin,

Zhou

et al. 2024

ApJ

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A rapidly rotating magnetar has long been assumed to inject energy into the ejecta through isotropic output energy in previous works. However, the output energy of a magnetar is anisotropic and a jet is generally presented in the rotational direction of a magnetar. In this paper, we present a consistent model of the energy injection from a magnetar, considering both the anisotropic magnetic dipole radiation and the jet’s ingredient (i.e., the late jet mentioned refers to the beamed magnetars wind). In the situation that the energy injection into the ejecta presents a significant effect on the ejecta’s emission, two facts are obtained. (1) For an observer in the equatorial direction, there is no significant difference between the light curves of the ejecta’s emission based on the consistent model and those obtained in previous works (i.e., based on the isotropic energy injection). (2) For an on jet-axis observer, however, the difference is significant, especially in the optical/U-band. If the jet is not present in the system, the rise of the optical/U-band light-curve is actually steeper than that in previous works because the output energy of the anisotropic magnetic dipole radiation is mainly in the equatorial direction. If the jet is present in the system, a bump from the cocoon (i.e., the late jet launch is expected to shock and heat-up the ejecta) may only appear in the optical/U-band light curve for a quasi-isotropic ejecta. Our results reveal that the anisotropic energy output of the magnetic dipole radiation and the jet’s ingredient should be well considered in modeling the ejecta emission by considering the energy injection from a magnetar. In addition, the optical/U-band light-curve may disclose the central engine of the burst.

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Sharp Decay of the Internal Plateau in Gamma-Ray Bursts: The Effect of a Cocoon's Thermal Photons on the Jet Emission

Cited by 2 publications

References 77 publications

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

The Effect of Anisotropic Energy Injection on the Ejecta Emission

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