Quark nova model for fast radio bursts

Shand, Zachary; Ouyed, Amir; Koning, Nico; Ouyed, Rachid

doi:10.1088/1674-4527/16/5/080

Cited by 30 publications

(26 citation statements)

References 44 publications

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“…Based on these typical characteristics, it has been suggested that these sources may originate at cosmological distances, corresponding to redshifts z of 0.5 to 1. If so, the isotropic total energy released in one FRB is inferred to be ∼ 10 38−40 erg, and the peak radio luminosity is estimated to be ∼ 10 42−43 erg s [11], neutron star mergers [12], white dwarf mergers [13], collapsing super-massive neutron stars [14,15], companions of extragalactic pulsars [16], asteroid collisions with neutron stars [17], quark nova [18], and dark matterinduced collapse of neutron stars [19]. All of these models considered FRBs as extragalactic burst sources.…”

Section: Introductionmentioning

confidence: 99%

Testing Einstein’s Equivalence Principle With Fast Radio Bursts

et al. 2015

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The accuracy of Einstein's Equivalence Principle (EEP) can be tested with the observed time delays between correlated particles or photons that are emitted from astronomical sources. Assuming as a lower limit that the time delays are caused mainly by the gravitational potential of the Milky Way, we prove that fast radio bursts (FRBs) of cosmological origin can be used to constrain the EEP with high accuracy. Taking FRB 110220 and two possible FRB/gamma-ray burst (GRB) association systems (FRB/GRB 101011A and FRB/GRB 100704A) as examples, we obtain a strict upper limit on the differences of the parametrized post-Newtonian parameter γ values as low as [γ(1.23 GHz) − γ(1.45 GHz)] < 4.36 × 10 −9 . This provides the most stringent limit up to date on the EEP through the relative differential variations of the γ parameter at radio energies, improving by 1 to 2 orders of magnitude the previous results at other energies based on supernova 1987A and GRBs.

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Section: Introductionmentioning

confidence: 99%

Testing Einstein’s Equivalence Principle With Fast Radio Bursts

et al. 2015

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“…This ejecta may be visible following the quark-nova either by interaction with surrounding material as a super-luminous or double-humped supernova, 5,6 or by the decay of unstable r-process isotopes as a fast radio burst. 7 Additional observational evidence for this r-process rich material may exist in the form of gravitationally bound fall-back material surrounding the quark-star. This fall-back material can either form a co-rotating shell, or a Keplerian disk depending on the period of the parent neutron star.…”

Section: Quark-novaementioning

confidence: 98%

Quark-nova compact remnants: Observational signatures in astronomical data and implications to compact stars

Ouyed¹,

Leany²,

Koning³

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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Quark-novae leave behind quark stars with a surrounding metal-rich fall-back (ring-like) material. These compact remnants have high magnetic fields and are misconstrued as magnetars; however, several observational features allow us to distinguish a quark star (left behind by a quark-nova) from a neutron star with high magnetic field. In our model, bursting activity is expected from intermittent accretion events from the surrounding fallback debris leading to X-ray bursts (in the case of a Keplerian ring) or gamma ray bursts (in the case of a co-rotating shell). The details of the spectra are described by a constant background X-ray luminosity from the expulsion of magnetic flux tubes which will be temporarily buried by bursting events caused by accretion of material onto the quark star surface. These accretion events emit high energy photons and heat up the quark star and surrounding debris leading to hot spots which may be observable as distinct blackbodies. Additionally, we explain observed spectral line features as atomic lines from r-process material and explain an observed anti-glitch in an AXP as the transfer of angular momentum from a surrounding Keplerian disk to the quark star.

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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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Quark nova model for fast radio bursts

Cited by 30 publications

References 44 publications

Testing Einstein’s Equivalence Principle With Fast Radio Bursts

Testing Einstein’s Equivalence Principle With Fast Radio Bursts

Quark-nova compact remnants: Observational signatures in astronomical data and implications to compact stars

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

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