The Allowed Parameter Space of a Long-lived Neutron Star as the Merger Remnant of GW170817

Ai, Shunke; Gao, He; Dai, Z. G.; Wu, Xue-Feng; Li, Ang; Zhang, Bing; Mu-zi, Li

doi:10.3847/1538-4357/aac2b7

Cited by 113 publications

(101 citation statements)

References 98 publications

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“…If the lifetime of SMNS is 155 d or longer, without violating the EM observational constraints, we should have B p < 8.5 × 10 10 G and ǫ < 1.0 × 10 −6 for WFF1, B p < 8.5 × 10 10 G and ǫ < 1.4 × 10 −6 for WFF2, B p < 8.5 × 10 10 G and ǫ < 7.1 × 10 −7 for AP4, B p < 8.7 × 10 10 G and ǫ < 5.9 × 10 −6 for BSK21, B p < 9.3 × 10 10 G and ǫ < 2.2 × 10 −5 for AP3 and B p < 1.0 × 10 11 G and ǫ < 3.4 × 10 −5 for DD2. The constraints on B p mainly come from the EM observations, which are roughly consistent with (slightly looser than) the constraints derived in our previous work (Ai et al 2018). In this paper, we only used the peak luminosity (or total kinetic energy) rather than the full lightcurve (used in Ai et al (2018)) to constrain the parameters.…”

Section: Constraints On the Ns Properties In The Mns Casessupporting

confidence: 72%

What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

Zhang

2020

ApJ

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The post-merger product of the first binary neutron star merger event detected in gravitational waves, GW170817, depends on neutron star equation of state (EoS) and is not well determined. We generally discuss the constraints one may pose on the maximum mass of a non-spinning neutron star, M TOV , based on the observations and some EoS-independent universal relations of rapidly-spinning neutron stars. If the merger product is a black hole after a brief hypermassive neutron star (HMNS) phase, we derive M TOV < 2.09 +0.06 −0.04 M ⊙ (2.09 +0.11 −0.09 M ⊙ ) at the 1σ (2σ) level. The cases for a massive neutron star (MNS), either a supra-massive neutron star (SMNS) or even a stable neutron star (SNS), are also allowed by the data. We derive 2.09 +0.06 −0.04 M ⊙ (2.09 +0.11 −0.09 M ⊙ ) ≤ M TOV < 2.43 +0.06 −0.04 M ⊙ (2.43 +0.10 −0.08 M ⊙ ) for the SMNS case and M TOV ≥ 2.43 +0.06 −0.04 M ⊙ (2.43 +0.10 −0.08 M ⊙ ) for the SNS case, at the 1σ (2σ) confidence level. In the MNS cases, we also discuss the constraints on the neutron star parameters (the dipolar magnetic field strength at the surface B p and the ellipticity ǫ) that affect the spindown history, by considering different MNS survival times, e.g. 300 s, 1 d, and 155 d after the merger, as suggested by various observational arguments. We find that once an SMNS is formed, without violating the EM observational constraints, there always exist a set of (B p , ǫ) parameters that allow the SMNS to survive for 300s, 1 d, 155 d, or even longer.

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Section: Constraints On the Ns Properties In The Mns Casessupporting

confidence: 72%

What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

Zhang

2020

ApJ

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“…Additionally, searches for enhanced late-time radio emission following 10 2 10 1 10 0 10 1 10 2 t (yr) SGRBs have placed limits on the fraction of BNS mergers that form magnetar remnants (Metzger & Bower 2014;Fong et al 2016;Horesh et al 2016), consistent with the estimates adopted in §3. The kinetic energy transferred to the ejecta via magnetic-dipole spin-down may be smaller than the total rotational energy of the magnetar due to inefficiencies in coupling the magnetar wind to the BNS merger/AIC ejecta (e.g., Bucciantini et al 2012), and hence we adopt E = 3 × 10 52 erg as a fiducial value 1 in 1 Even this energy deposition would be overestimated if the NS is sufficiently deformed into a non-axisymmetric shape such that that GW spin-down dominates over magnetic-dipole spin-down (Ai et al 2018); however, this requires extreme NS ellipticities, which may not be sustainable given that the required magnetic field configurations are not MHD stable except in a narrow region of parameter space ). Figure 3 show a simplified model for the radio light curve produced by the interaction of the magnetar-accelerated ejecta with the ISM, using the formulation of Nakar & Piran (2011) and assuming M ej = 0.1M , E = 3 × 10 52 erg, v ej given by Equation 4, and different ISM densities.…”

Section: Ejecta Radio Transparency Afterglow Andmentioning

confidence: 99%

Fast Radio Bursts from Magnetars Born in Binary Neutron Star Mergers and Accretion Induced Collapse

Margalit

Berger

Metzger

2019

ApJ

161

151

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Recently born magnetars are promising candidates for the engines powering fast radio bursts (FRBs). The focus thus far has been placed on millisecond magnetars born in rare core-collapse explosions, motivated by the star forming dwarf host galaxy of the repeating FRB 121102, which is remarkably similar to the hosts of superluminous supernovae (SLSNe) and long gamma-ray bursts (LGRB). However, long-lived magnetars may also be created in binary neutron star (BNS) mergers, in the small subset of cases with a sufficiently low total mass for the remnant to avoid collapse to a black hole, or in the accretion-induced collapse (AIC) of a white dwarf. A BNS FRB channel will be characterized by distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate a similar host population, although possibly different offset distribution for AIC events. We show that both the BNS and AIC channels are consistent with the recently reported FRB 180924, localized by ASKAP to a massive quiescent host galaxy with an offset of about 1.4 effective radii. FRBs from magnetars born in BNS mergers and AIC will be accompanied by persistent synchrotron radio emission on timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel. Using models calibrated to FRB 121102, we make predictions for the dispersion measure, rotation measure, and persistent radio emission from magnetar FRB sources born in BNS mergers or AIC, and show these are consistent with upper limits from FRB 180924 for reasonable parameters. Depending on the rate of AIC, and the fraction of BNS mergers leaving long-lived stable magnetars, the birth rate of repeating FRB sources associated with older stellar populations could be comparable to that of the core-collapse channel. We also discuss potential differences in the repetition properties of these channels, as a result of differences in the characteristic masses and magnetic fields of the magnetars.

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“…The only remaining variables in Equations (8) and (14) are related to the NS EoS. Here, we consider 12 EoSs that are usually discussed in the literatures (see Table 1), and EoS parameters are taken from Lasky et al (2014), , Li et al (2016), and Ai et al (2018). Figure 2 and 3 show the t col as a function of protomagnetar mass (M p ) for GRB 101219A and GRB 160821B, respectively.…”

Section: Constraining the Eosmentioning

confidence: 99%

“…If this is the case, the GW radiation of a newly born magnetar can be produced via either a mass quadrupole deformation with ellipticity ε for an NS rotating as a rigid body or an r -mode fluid oscillation with amplitude α Lindblom et al 1998;Andersson & Kokkotas 2001;Zhang & Mészáros 2001;Owen 2010;Yu et al 2010;Fan et al 2013;Lasky 2015;Ho 2016;Lasky & Glampedakis 2016;Lü et al 2017). These GW signals are too weak to be detected by the current Advanced LIGO and Advanced Virgo observatories (Alford & Schwenzer 2014, 2015Abbott et al 2017c;Lü et al 2017Lü et al , 2019Ai et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Constraining the Nuclear Equation of State via Gravitational-wave Radiation of Short Gamma-Ray Burst Remnants

Lin

Lü

Rice

et al. 2020

ApJ

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The observed internal plateau of X-ray emission in some short gamma-ray bursts (GRBs) suggests the formation of a remnant supramassive magnetar following a double neutron star (NS) merger. In this paper, we assume that the rotational energy is lost mainly via gravitational-wave (GW) radiation instead of magnetic dipole (MD) radiation, and present further constraints on the NS nuclear equation of state (EoS) via mass quadrupole deformation and r -mode fluid oscillations of the magnetar. We present two short GRBs with measured redshifts, 101219A and 160821B, whose X-ray light curves exhibit an internal plateau. This suggests that a supramassive NS may survive as the central engine. By considering 12 NS EoSs, within the mass quadrupole deformation scenario we find that the GM1, DD2, and DDME2 models give an M p band falling within the 2σ region of the proto-magnetar mass distribution for ε = 0.01. This is consistent with the constraints from the MD radiation dominated model of rotational energy loss. However, for an r -mode fluid oscillation model with α = 0.1 the data suggest that the NS EOS is close to the Shen and APR models, which is obviously different from the MD radiation dominated and mass quadrupole deformation cases.

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The Allowed Parameter Space of a Long-lived Neutron Star as the Merger Remnant of GW170817

Cited by 113 publications

References 98 publications

What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

Fast Radio Bursts from Magnetars Born in Binary Neutron Star Mergers and Accretion Induced Collapse

Constraining the Nuclear Equation of State via Gravitational-wave Radiation of Short Gamma-Ray Burst Remnants

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