Reverse shock emission driven by post-merger millisecond magnetar winds: Effects of the magnetization parameter

Liu, Liang-Duan; Wang, L. J.; Dai, Z. G.

doi:10.1051/0004-6361/201628072

Cited by 7 publications

(6 citation statements)

References 58 publications

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“…Inspection of Figure 8 of Kotera et al (2013) indicates that this could imply average magnetar photon energies ∼ 10 − 100 keV, in agreement with observation (Hester 2008). Theoretically, magnetar radiation depends on several parameters, e.g., magnetic field, rotation period, angle between rotation axis and magnetic axis, and theorists are still struggling to unequivocally predict its spectrum energy distribution (Kennel & Coroniti 1984a,b;Lyubarsky & Kirk 2001;Wang & Dai 2013;Kargaltsev et al 2015;Murase et al 2015;Wang et al 2015aWang et al , 2016aLiu et al 2016a).…”

Section: Discussionsupporting

confidence: 74%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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Section: Discussionsupporting

confidence: 74%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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“…It is usually believed that the central engine of GRBs are black holes (Popham et al 1999;Narayan et al 2001;Kohri & Mineshige 2002;Liu et al 2007;Song et al 2016) or magnetars (Usov 1992;Dai & Lu 1998a,b;Zhang & Dai 2008, 2010Giacomazzo & Perna 2013;Giacomazzo et al 2015). However, since it is currently infeasible to identify the GRB central engine directly because of the cosmological distance scales of GRBs (Kumar & Zhang 2015), the researchers instead pursue indirect signatures of black holes (Geng et al 2013;Wu et al 2013;Yu et al 2015) and magnetars (Dai et al 2006;Gao et al 2013;Wang & Dai 2013;Zhang 2013;Yu et al 2013;Metzger & Piro 2014;Wang et al 2015aWang et al , 2016aLi & Yu 2016;Liu et al 2016) that powers the energetic GRBs. Growing indirect observational evidence suggests that magnetars could act as the central engine of both LGRBs and SGRBs (Dai et al 2006;Rowlinson et al 2010Rowlinson et al , 2013Dai & Liu 2012;Wang & Dai 2013;Wu et al 2014;Gao et al 2015;Greiner et al 2015).…”

Section: Discussionmentioning

confidence: 99%

SOLVING THE ⁵⁶Ni PUZZLE OF MAGNETAR-POWERED BROAD-LINED TYPE IC SUPERNOVAE

Wang

Han

et al. 2016

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are a subclass of rare core collapse SNe whose energy source is debated in the literature. Recently a series of investigations on SNe Ic-BL with the magnetar (plus 56 Ni) model were carried out. Evidence for magnetar formation was found for the well-observed SNe Ic-BL 1998bw and 2002ap. In this paper we systematically study a large sample of SNe Ic-BL not associated with gamma-ray bursts. We use photospheric velocity data determined in a homogeneous way. We find that the magnetar+ 56 Ni model provides a good description of the light curves and velocity evolution of our sample of SNe Ic-BL, although some SNe (not all) can also be described by the pure-magnetar model or by the two-component pure-56 Ni model (3 out of 12 are unlikely explained by two-component model). In the magnetar+ 56 Ni model, the amount of 56 Ni required to explain their luminosity is significantly reduced, and the derived initial explosion energy is, in general, in accordance with neutrino heating. Some correlations between different physical parameters are evaluated and their implications regarding magnetic field amplification and the total energy reservoir are discussed.

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“…The number density and the internal energy density of Region 3, n 3 and e 3 , can be obtained by the shock jump conditions (for the situation of σ = 0, Coroniti 1990;Zhang & Kobayashi 2005;Mao et al 2010;Liu et al 2016) as…”

Section: Hydrodynamics and Radiationmentioning

confidence: 99%

Brightening X-Ray/Optical/Radio Emission of GW170817/SGRB 170817A: Evidence for an Electron–Positron Wind from the Central Engine?

Geng

Dai

Huang

et al. 2018

ApJL

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Recent follow-up observations of the binary neutron star (NS) merging event GW170817/SGRB 170817A reveal that its X-ray/optical/radio emissions are brightening continuously up to ∼ 100 days post-merger. This late-time brightening is unexpected from the kilonova model or the off-axis top-hat jet model for gamma-ray burst afterglows. In this paper, by assuming that the merger remnant is a long-lived NS, we propose that the interaction between an electron-positron-pair (e + e − ) wind from the central NS and the jet could produce a long-lived reverse shock, from which a new emission component would rise and can interpret current observations well. The magnetic-field-induced ellipticity of the NS is taken to be 4×10 −5 in our modeling, so that the braking of the NS is mainly through the gravitational wave (GW) radiation rather than the magnetic dipole radiation, and the emission luminosity at early times would not exceed the observational limits. In our scenario, since the peak time of the brightening is roughly equal to the spin-down time scale of the NS, the accurate peak time may help constrain the ellipticity of the remnant NS. We suggest that radio polarization observations of the brightening would help to distinguish our scenario from other scenarios. Future observations on a large sample of short gamma-ray burst afterglows or detections of GW signals from merger remnants would test our scenario.

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Reverse shock emission driven by post-merger millisecond magnetar winds: Effects of the magnetization parameter

Cited by 7 publications

References 58 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

SOLVING THE ⁵⁶Ni PUZZLE OF MAGNETAR-POWERED BROAD-LINED TYPE IC SUPERNOVAE

Brightening X-Ray/Optical/Radio Emission of GW170817/SGRB 170817A: Evidence for an Electron–Positron Wind from the Central Engine?

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Reverse shock emission driven by post-merger millisecond magnetar winds: Effects of the magnetization parameter

Cited by 7 publications

References 58 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

SOLVING THE 56Ni PUZZLE OF MAGNETAR-POWERED BROAD-LINED TYPE IC SUPERNOVAE

Brightening X-Ray/Optical/Radio Emission of GW170817/SGRB 170817A: Evidence for an Electron–Positron Wind from the Central Engine?

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Product

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SOLVING THE ⁵⁶Ni PUZZLE OF MAGNETAR-POWERED BROAD-LINED TYPE IC SUPERNOVAE