A model of neutron-star–white-dwarf collision for fast radio bursts

Ling, Xiang

doi:10.1007/s10509-018-3462-3

Cited by 29 publications

(20 citation statements)

References 70 publications

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“…Dokuchaev and Eroshenko (2017) take this argument one step further and predict FRBs from binary neutron star collisions only in or near the center of densely packed stellar clusters in galactic nuclei, and Iwazaki (2015) theorizes that FRBs are generated in the collision between a neutron star and a dense axion star. Alternatively, Liu (2017) proposes that FRBs are produced in neutron star -white dwarf collisions.…”

Section: Colliding Neutron Star Modelsmentioning

confidence: 99%

Fast radio bursts

Petroff

Hessels

Lorimer

2019

Astron Astrophys Rev

618

471

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The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar to the individual pulses from pulsars, their large dispersive delays suggest that they originate from far outside the Milky Way and hence are many ordersof-magnitude more luminous. While most FRBs appear to be one-off, perhaps cataclysmic events, two sources are now known to repeat and thus clearly have a longer-lived central engine. Beyond understanding how they are created, there is also the prospect of using FRBs -as with pulsars -to probe the extremes of the Universe as well as the otherwise invisible intervening medium. Such studies will be aided by the high implied all-sky event rate: there is a detectable FRB roughly once every minute occurring somewhere on the sky. The fact that less than a hundred FRB sources have been discovered in the last decade is largely due to the small fields-of-view of current radio telescopes. A new generation of wide-field instruments is now coming online, however, and these will be capable of detecting multiple FRBs per day. We are thus on the brink of further breakthroughs in the short-duration radio transient phase space, which will be critical for differentiating between the many proposed theories for the origin of FRBs. In this review, we give an observational and theoretical introduction at a level that is accessible to astronomers entering the field.

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Section: Colliding Neutron Star Modelsmentioning

confidence: 99%

Fast radio bursts

Petroff

Hessels

Lorimer

2019

Astron Astrophys Rev

618

471

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“…In addition to the well-observed MSP population in GCs, four young pulsars (with estimated ages  100 Myr) are observed in Galactic GCs, suggesting that young NSs are formed at late times in GCs through some mechanism (e.g., Tauris et al 2013;Boyles et al 2011). Binary WD mergers (e.g., King et al 2001;Schwab et al 2016;Kremer et al 2021), accretion-induced collapse (AIC) of WDs in binaries (e.g., Nomoto & Kondo 1991;Tauris et al 2013), binary NS mergers (e.g., Rosswog et al 2003;Giacomazzo & Perna 2013), and/or NS-WD mergers (e.g., Liu 2018;Zhong & Dai 2020) may all lead to young NS formation in clusters. Thus, a number of scenarios may operate in GCs that could produce a progenitor of the M81 FRB.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Formation Channels for Fast Radio Bursts in Globular Clusters

Kremer

Piro

2021

ApJL

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The repeating fast radio burst (FRB) localized to a globular cluster (GC) in M81 challenges our understanding of FRB models. In this Letter, we explore dynamical formation scenarios for objects in old GCs that may plausibly power FRBs. Using N-body simulations, we demonstrate that young neutron stars (NSs) may form in GCs at a rate of up to ∼50 Gpc −3 yr −1 through a combination of binary white dwarf (WD) mergers, WD-NS mergers, binary NS mergers, and accretion-induced collapse of massive WDs in binary systems. We consider two FRB emission mechanisms: First, we show that a magnetically powered source (e.g., a magnetar with field strength 10 14 G) is viable for radio emission efficiencies 10 −4 . This would require magnetic activity lifetimes longer than the associated spin-down timescales and longer than empirically constrained lifetimes of Galactic magnetars. Alternatively, if these dynamical formation channels produce young rotation-powered NSs with spin periods of ∼10 ms and magnetic fields of ∼10 11 G (corresponding to spin-down lifetimes of 10 5 yr), the inferred event rate and energetics can be reasonably reproduced for order unity duty cycles. Additionally, we show that recycled millisecond pulsars or low-mass X-ray binaries similar to those well-observed in Galactic GCs may also be plausible channels, but only if their duty cycle for producing bursts similar to the M81 FRB is small.

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“…Models of non-repeating FRBs include a collapse of a neutron star (e.g., Fuller & Ott 2015;Falcke & Rezzolla 2014;Shand et al 2016), NS-asteroid collision (Geng & Huang 2015), pulsar-black hole (BH) interaction (Bhattacharyya 2017), merger of compact objects (e.g., Zhang 2016;Liu et al 2016;Mingarelli et al 2015;Totani 2013;Liu 2018;Li et al 2018;Kashiyama et al 2013;Yamasaki et al 2018), NS-supernova (SN) interaction (Egorov & Postnov 2009), AGN jet-cloud interaction (e.g., Romero et al 2016) and SN remnant powered by a flare from a magnetar (e.g., Popov & Postnov 2010;Lyubarsky 2014;Murase et al 2016).…”

Section: Implications On Frb Modelsmentioning

confidence: 99%

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

Hashimoto

Goto

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Fast radio bursts (FRBs) are mysterious radio bursts with a time scale of approximately milliseconds. Two populations of FRB, namely repeating and non-repeating FRBs, are observationally identified. However, the differences between these two and their origins are still cloaked in mystery. Here we show the time-integrated luminosityduration (L ν -w int,rest ) relations and luminosity functions (LFs) of repeating and nonrepeating FRBs in the FRB Catalogue project. These two populations are obviously separated in the L ν -w int,rest plane with distinct LFs, i.e., repeating FRBs have relatively fainter L ν and longer w int,rest with a much lower LF. In contrast with non-repeating FRBs, repeating FRBs do not show any clear correlation between L ν and w int,rest . These results suggest essentially different physical origins of the two. The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron-star mergers and accretion-induced collapse (AIC) of white dwarfs, and are consistent with those of soft gamma-ray repeaters (SGRs), type Ia supernovae, magnetars, and white-dwarf mergers. This indicates two possibilities: either (i) faint non-repeating FRBs originate in neutron-star mergers or AIC and are actually repeating during the lifetime of the progenitor, or (ii) faint non-repeating FRBs originate in any of SGRs, type Ia supernovae, magnetars, and white-dwarf mergers. The bright ends of LFs of repeating and non-repeating FRBs are lower than any candidates of progenitors, suggesting that bright FRBs are produced from a very small fraction of the progenitors regardless of the repetition. Otherwise, they might originate in unknown progenitors.

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A model of neutron-star–white-dwarf collision for fast radio bursts

Cited by 29 publications

References 70 publications

Fast radio bursts

Fast radio bursts

Dynamical Formation Channels for Fast Radio Bursts in Globular Clusters

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

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