Pulsar revival in neutron star mergers: multimessenger prospects for the discovery of pre-merger coherent radio emission

Cooper, A. J.; Gupta, Om; Wadiasingh, Zorawar; Wijers, R. A. M. J.; Boersma, Oliver M.; Andreoni, Igor; Rowlinson, A.; Gourdji, K.

doi:10.1093/mnras/stac3580

Cited by 8 publications

(19 citation statements)

References 217 publications

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“…There are three one-off FRBs with periodic subpulses, i.e., FRBs 20191221A (216.8 ms), 20210206A (2.8 ms), and 20210213A (10.7 ms), reported by CHIME/FRB Collaboration et al (2022), where the period signal significance of FRB 20191221A (6.5σ) is higher than that of FRB 20210206A (1.3σ) and FRB 20210213A (2.4σ). The origin of their periodicity is an open question (Beniamini & Kumar 2023;Wang et al 2023;Cooper et al 2023). It is proposed that such kinds of FRBs (like FRB 20191221A and FRB 20210213A) may be produced during the inspiral phase of a BNS merger (Most & Philippov 2022; CHIME/FRB Collaboration et al 2022), and we noted that FRB 20210206A is disfavored in a BNS-merger scenario as its expected period derivative is not consistent with the observed subpulse separation (CHIME/ FRB Collaboration et al 2022).…”

Section: Properties Of the Bnss For Two One-off Frbsmentioning

confidence: 66%

“…This scenario has been confirmed by general relativistic magnetohydrodynamic simulations (e.g., Palenzuela et al 2013aPalenzuela et al , 2013bPonce et al 2014;Most & Philippov 2020). Compared with the postmerger multiband emission, radiation signals from the premerger BNS may provide more detailed information about the equation of state for the NSs (Neill et al 2022;Pan et al 2022;Zhang et al 2022) and magnetospheric interaction in a BNS system (Lyutikov 2023;Pan et al 2022;Cooper et al 2023).…”

Section: Introductionmentioning

confidence: 64%

“…To obtain a credible event rate of BNS-merger-originated FRBs, i.e., BNS mergers with both NSs' magnetic field strengths being higher than 10 12 G, we use population synthesis and adopt decaying magnetic fields for the NSs to study the event rate of BNS mergers in Section 3. We also provide the event rate of BNS mergers with at least one magnetized NS (>10 12 G), which could be useful in other scenarios, e.g., Wang et al (2016) and Cooper et al (2023).…”

Section: Properties Of the Bnss For Two One-off Frbsmentioning

confidence: 99%

“…Wang et al (2016) found that a unipolar inductor model (Goldreich & Lynden-Bell 1969;Lai 2012;Piro 2012) with a highly magnetized primary NS (B  10 12 G) and a weakly magnetized companion could produce an FRB by accelerating electrons in coherent slices. Cooper et al (2023) investigated pulsar-like emission within the polar gap model (Ruderman & Sutherland 1975;Daugherty & Harding 1982) and showed that coherent millisecond radio bursts could be detected at gigaparsec distances by next-generation radio facilities if one NS has a magnetic field higher than 10 12 G. Fast magnetosonic waves have been considered in magnetars (Lyubarsky 2020;Mahlmann et al 2022) and double NS systems (Most & Philippov 2023) as a radio emission mechanism for FRBs. Most & Philippov (2023) presented the detailed behavior of the flare arising from the magnetic reconnection in the common magnetospheres of BNS with magnetic fields of ∼10 11 G, and demonstrated that if the flare interacts with the orbital current sheet, it could produce a radio transient with a submillisecond quasi-periodic structure like FRB 20201020A (Pastor-Marazuela et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Event Rate of Fast Radio Bursts from Binary Neutron Star Mergers

Chen

Lin

et al. 2023

ApJ

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It is proposed that a one-off fast radio burst (FRB) with periodic structure may be produced during the inspiral phase of a binary neutron star (BNS) merger. In this paper, we study the event rate of such kind of FRB. We first investigate the properties of two one-off FRBs with periodic structure (i.e., FRB 20191221A and FRB 20210213A) in this scenario, by assuming a fast magnetosonic wave is responsible for their radio emission. For the luminosities and periods of these bursts, it is found that for the NSs in the premerger BNS, magnetic field strengths of B ≳ 1012 G are required. This is relatively high compared with those of most of the BNSs observed in our Galaxy, of which their magnetic fields are around 109 G. Since the observed BNSs in our Galaxy are binaries that have not suffered a merger, a credible event rate of BNS-merger-originated FRBs should be estimated by considering the evolution of both the BNS systems and their magnetic fields. Based on population synthesis and adopting decaying magnetic fields of the NSs, we estimate the event rate of BNS mergers relative to their final magnetic fields. We find that rapidly merging BNSs tend to merge with high magnetization, and the event rate of BNS-merger-originated FRBs, i.e., BNS mergers with both NSs’ magnetic fields being higher than 1012 G, is ∼8 × 104 yr−1 (19% of all BNS mergers) for redshifts z < 1.

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Section: Properties Of the Bnss For Two One-off Frbsmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 64%

Section: Properties Of the Bnss For Two One-off Frbsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Event Rate of Fast Radio Bursts from Binary Neutron Star Mergers

Chen

Lin

et al. 2023

ApJ

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“…In other scenarios, the precursor is related to the strong interaction between the two compact objects right before they merge. Luminous high-energy emission is predicted by models that involve the shattering of the NS crust during the inspiral phase (e.g., Tsang et al 2012;Palenzuela et al 2013;Neill et al 2021;Suvorov & Kokkotas 2021) or the magnetospheric interactions between the NS and another compact object (e.g., McWilliams & Levin 2011;Most & Philippov 2020;Beloborodov 2021;Cooper et al 2023). Schnittman et al (2018) suggested that, regardless of their power source, precursors produced in the premerger phase should display a modulated temporal profile induced by the stars' orbital motion.…”

Section: Introductionmentioning

confidence: 99%

A Luminous Precursor in the Extremely Bright GRB 230307A

Dichiara,

Tsang,

Troja

et al. 2023

ApJL

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GRB 230307A is an extremely bright long-duration GRB with an observed gamma-ray fluence of ≳3 × 10−3 erg cm−2 (10–1000 keV), second only to GRB 221009A. Despite its long duration, it is possibly associated with a kilonova, thus resembling the case of GRB 211211A. In analogy with GRB 211211A, we distinguish three phases in the prompt gamma-ray emission of GRB 230307A: an initial short duration, spectrally soft emission; a main long duration, spectrally hard burst; and a temporally extended and spectrally soft tail. We interpret the initial soft pulse as a bright precursor to the main burst and compare its properties with models of precursors from compact binary mergers. We find that to explain the brightness of GRB 230307A, a magnetar-like (≳1015 G) magnetic field should be retained by the progenitor neutron star. Alternatively, in the postmerger scenario, the luminous precursor could point to the formation of a rapidly rotating massive neutron star.

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MWA rapid follow-up of gravitational wave transients: Prospects for detecting prompt radio counterparts

Tian,

Anderson,

Cooper

et al. 2023

Publ. Astron. Soc. Aust.

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We present and evaluate the prospects for detecting coherent radio counterparts to gravitational wave (GW) events using Murchison Widefield Array (MWA) triggered observations. The MWA rapid-response system, combined with its buffering mode ( $\sim$ 4 min negative latency), enables us to catch any radio signals produced from seconds prior to hours after a binary neutron star (BNS) merger. The large field of view of the MWA ( $\sim$ $1\,000\,\textrm{deg}^2$ at 120 MHz) and its location under the high sensitivity sky region of the LIGO-Virgo-KAGRA (LVK) detector network, forecast a high chance of being on-target for a GW event. We consider three observing configurations for the MWA to follow up GW BNS merger events, including a single dipole per tile, the full array, and four sub-arrays. We then perform a population synthesis of BNS systems to predict the radio detectable fraction of GW events using these configurations. We find that the configuration with four sub-arrays is the best compromise between sky coverage and sensitivity as it is capable of placing meaningful constraints on the radio emission from 12.6% of GW BNS detections. Based on the timescales of four BNS merger coherent radio emission models, we propose an observing strategy that involves triggering the buffering mode to target coherent signals emitted prior to, during or shortly following the merger, which is then followed by continued recording for up to three hours to target later time post-merger emission. We expect MWA to trigger on $\sim$ $5-22$ BNS merger events during the LVK O4 observing run, which could potentially result in two detections of predicted coherent emission.

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Pulsar revival in neutron star mergers: multimessenger prospects for the discovery of pre-merger coherent radio emission

Cited by 8 publications

References 217 publications

Event Rate of Fast Radio Bursts from Binary Neutron Star Mergers

Event Rate of Fast Radio Bursts from Binary Neutron Star Mergers

A Luminous Precursor in the Extremely Bright GRB 230307A

MWA rapid follow-up of gravitational wave transients: Prospects for detecting prompt radio counterparts

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