Fast Radio Bursts: Collisions Between Neutron Stars and Asteroids/Comets

Geng, Jin-Jun; Huang, Yun‐Feng

doi:10.1088/0004-637x/809/1/24

Cited by 137 publications

(121 citation statements)

References 43 publications

Supporting

Mentioning

118

Contrasting

Unclassified

Order By: Relevance

“…Related ideas have included the interaction of pulsars with planets, 39 asteroids or comets. 40,41 Less exotic models, applicable only if FRB are not at cosmological distances, have appealed to events like stellar flares. The observed short durations of FRB imply small emitting regions, because emission over larger regions would, by a spread in radiation travel times ∆t, produce longer pulses; in the absence of relativistic bulk (including phase) motion ∆t ≥ ∆r/c, where ∆t is the observed burst duration and ∆r is the dimension of the radiating region (properly, its dimension along the direction of radiation).…”

Section: What Are They?mentioning

confidence: 99%

Fast radio bursts — A brief review: Some questions, fewer answers

Katz¹

2016

Mod. Phys. Lett. A

125

126

View full text Add to dashboard Cite

Fast radio bursts (FRBs) are millisecond bursts of radio radiation at frequencies of about 1 GHz, recently discovered in pulsar surveys. They have not yet been definitively identified with any other astronomical object or phenomenon. The bursts are strongly dispersed, indicating passage through a high column density of low density plasma. The most economical interpretation is that this is the interglactic medium, indicating that FRB are at "cosmological" distances with redshifts in the range 0.3-1.3. Their inferred brightness temperatures are as high as 10 37 • K, implying coherent emission by "bunched" charges, as in radio pulsars. I review the astronomical sites, objects and emission processes that have been proposed as the origin of FRB, with particular attention to soft gamma repeaters (SGRs) and giant pulsar pulses.

show abstract

Section: What Are They?mentioning

confidence: 99%

Fast radio bursts — A brief review: Some questions, fewer answers

Katz¹

2016

Mod. Phys. Lett. A

125

126

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…The repeating burst is more likely to originate from young remnants of stellar collapses, neutron stars or black holes (Katz 2016a), e.g. soft gamma repeaters (Pen & Connor 2015;Katz 2016c), giant pulse from young pulsars (Keane et al 2012;Katz 2016b), and the interaction of pulsars with planets (Mottez & Zarka 2014), asteroids or comets (Geng & Huang 2015;Dai et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A Fast Radio Burst Search Method for VLBI Observation

Liu¹,

Tong²,

Zheng³

et al. 2018

View full text Add to dashboard Cite

We introduce the cross spectrum based FRB (Fast Radio Burst) search method for VLBI observation. This method optimizes the fringe fitting scheme in geodetic VLBI data post processing, which fully utilizes the cross spectrum fringe phase information and therefore maximizes the power of single pulse signals. Working with cross spectrum greatly reduces the effect of radio frequency interference (RFI) compared with using auto spectrum. Single pulse detection confidence increases by cross identifying detections from multiple baselines. By combining the power of multiple baselines, we may improve the detection sensitivity. Our method is similar to that of coherent beam forming, but without the computational expense to form a great number of beams to cover the whole field of view of our telescopes. The data processing pipeline designed for this method is easy to implement and parallelize, which can be deployed in various kinds of VLBI observations. In particular, we point out that VGOS observations are very suitable for FRB search.

show abstract

Fast Radio Bursts: Collisions Between Neutron Stars and Asteroids/Comets

Cited by 137 publications

References 43 publications

Fast radio bursts — A brief review: Some questions, fewer answers

Fast radio bursts — A brief review: Some questions, fewer answers

Testing Einstein’s Equivalence Principle With Fast Radio Bursts

A Fast Radio Burst Search Method for VLBI Observation

Contact Info

Product

Resources

About