Fast Radio Bursts as Crustal Dynamical Events Induced by Magnetic Field Evolution in Young Magnetars

Horvath, J. E.; Moraes, P. H. R. S.; Avellar, Marcio G. B. de; Rocha, L. S.

doi:10.1088/1674-4527/ac440f

Cited by 2 publications

(1 citation statement)

References 103 publications

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“…Solitons can radiate via several conceivable emission mechanisms because of their strong nonlinearity and long time stability. The coherent curvature radiation of cavitons moving along curved magnetic field lines of pulsars is a widely considered radio emission mechanism of neutron stars (Weatherall & Benford 1991;Melikidze et al 2000Melikidze et al , 2014Gil et al 2004;Mitra et al 2009;Mitra 2017;Rahaman et al 2020b;Horvath et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Streaming instability in neutron star magnetospheres: No indication of soliton-like waves

Benáček,

Muñoz,

Büchner

et al. 2024

A&A

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Coherent radiation of pulsars, magnetars, and fast radio bursts could, in theory, be interpreted as radiation from solitons and soliton-like waves. Solitons are meant to contain a large number of electric charges confined on long timescales and can radiate strongly via coherent curvature emission. However, solitons are also known to undergo a wave collapse, which casts doubts on the correctness of the soliton radio emission models of neutron stars. We investigated the evolution of the caviton type of solitons self-consistently formed by the relativistic streaming instability and compared their apparent stability in 1D calculations with more generic 2D cases, in which the solitons are seen to collapse. Three representative cases of beam Lorentz factors and plasma temperatures were studied to obtain soliton dispersion properties. We utilized 1D electrostatic and 2D electromagnetic relativistic particle-in-cell simulations at kinetic microscales. We find that no solitons are generated by the streaming instability in the 2D simulations. Only superluminal L-mode (relativistic Langmuir) waves are produced during the saturation of the instability, but these waves have smaller amplitudes than the waves in the 1D simulations. The amplitudes tend to decrease after the instability has saturated, and only waves close to the light line, $ = c k$ remain. Solitons in the 1D approach are stable for $ b 60$, but they disappear for low beam Lorentz factors, $ b Our examples show that the superluminal soliton branch that is formed in 1D simulations will not be generated by the relativistic streaming instability when more dimensional degrees of freedom are present. The soliton model cannot, therefore, be used to explain the coherent radiation of pulsars, magnetars, and fast radio bursts --- unless one can show that there are alternative plasma mechanisms for the soliton generation.

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Section: Introductionmentioning

confidence: 99%

Streaming instability in neutron star magnetospheres: No indication of soliton-like waves

Benáček,

Muñoz,

Büchner

et al. 2024

A&A

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Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

Laha

Younes

Wadiasingh

et al. 2022

ApJ

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FRB 180301 is one of the most actively repeating fast radio bursts (FRBs) that has shown polarization angle changes in its radio burst emission, an indication for their likely origin in the magnetosphere of a highly magnetized neutron star. We carried out a multiwavelength campaign with the FAST radio telescope and NICER X-ray observatory to investigate any possible X-ray emission temporally coincident with the bright radio bursts. The observations took place on 2021 March 4, 9 and 19. We detected five bright radio bursts with FAST, four of which were strictly simultaneous with the NICER observations. The peak flux density of the radio bursts ranged between 28 and 105 mJy, the burst fluence between 27 and 170 mJy ms, and the burst durations between 1.7 and 12.3 ms. The radio bursts from FRB 180301 exhibited a complex time domain structure, and subpulses were detected in individual bursts, with no significant circular polarization. The linear degree of polarization in the L band reduced significantly compared to the 2019 observations. We do not detect any X-ray emission in excess of the background during the 5, 10, 100 ms, 1 and 100 s time intervals at/around the radio-burst barycenter-corrected arrival times, at a > 5σ confidence level. The 5σ upper limits on the X-ray (a) persistent flux is <7.64 × 10−12 erg cm−2 s−1, equivalent to L X < 2.50 × 1045 erg s−1 and (b) 5 ms fluence is <2 × 10−11 erg cm−2, at the radio burst regions. Using the 5 ms X-ray fluence upper limit, we can estimate the radio efficiency η R/X ≡ L radio/L X−ray ≳ 10−8. The derived lower limit on η R/X is consistent with both magnetospheric models and synchrotron maser models involving relativistic shocks.

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Fast Radio Bursts as Crustal Dynamical Events Induced by Magnetic Field Evolution in Young Magnetars

Cited by 2 publications

References 103 publications

Streaming instability in neutron star magnetospheres: No indication of soliton-like waves

Streaming instability in neutron star magnetospheres: No indication of soliton-like waves

Simultaneous View of FRB 180301 with FAST and NICER during a Bursting Phase

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