A comparison between repeating bursts of FRB 121102 and giant pulses from Crab pulsar and its applications

Lyu, Fen; Meng, Yan-Zhi; Tang, Zhen-Fan; Li, Ye; Wei, Jun-Jie; Geng, Jin-Jun; Lin, Lin; Deng, Can-Min; Wu, Xue-Feng

doi:10.1007/s11467-020-1039-4

Cited by 21 publications

(11 citation statements)

References 67 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Cordes & Wasserman 2016). The giant pulses of Crab pulsar also show a power-law distribution (Popov & Stappers 2007;Lyu et al 2021). A power-law distribution of energy is a natural predication of self-organized criticality theory (Bak et al 1987;Aschwanden 2011).…”

Section: Energy Distributionmentioning

confidence: 98%

Energy and waiting time distributions of FRB 121102 observed by FAST

Zhang,

Wang,

et al. 2021

Preprint

View full text Add to dashboard Cite

The energy and waiting time distributions are important properties to understand the physical mechanism of repeating fast radio bursts (FRBs). Recently, Five-hundredmeter Aperture Spherical radio Telescope (FAST) detected the largest sample of FRB 121102, containing 1652 bursts. The energy distribution at high-energy range (> 10 38 erg) can be fitted with a single power-law function with an index of −1.86. However, the distribution at low-energy range deviates from the power-law function. The energy distributions of high-energy bursts at different epochs are inconsistent. We find the power-law index of −1.70 for early bursts and −2.60 for later bursts. For bursts observed in a single day, a linear repetition pattern is found. We use the Weibull function to fit the waiting time distribution. The shape parameter k = 0.72 +0.01 −0.02 and the event rate r = 734.47 +29.04 −27.58 day −1 are derived. If the waiting times with δ t < 28 s are excluded, the burst behavior can be described by a Poisson process. The best-fitting values of k are slightly different for low-energy and high-energy bursts. The event rates change significantly across the observing time, while the shape parameters k vary slightly in different days.

show abstract

Section: Energy Distributionmentioning

confidence: 98%

Energy and waiting time distributions of FRB 121102 observed by FAST

Zhang,

Wang,

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…It has also become simpler to define the FRB class by its luminosity as more FRBs are associated with host galaxies. Therefore, we propose an FRB radio spectral energy threshold of 10 29 erg Hz −1 , which includes all FRBs and excludes all other millisecond radio transients associated with well defined Galactic classes (e.g., Crab giant pulses; Cordes et al 2004;Lyu et al 2021). With this definition, a repeating FRB is defined as any source with multiple bursts with energy greater than 10 29 erg Hz −1 .…”

Section: Frb and Prs Populationsmentioning

confidence: 99%

On the Fast Radio Burst and Persistent Radio Source Populations

Law,

Connor,

Aggarwal

2021

Preprint

View full text Add to dashboard Cite

The first Fast Radio Burst (FRB) to be precisely localized was associated with a luminous persistent radio source (PRS). Recently, a second FRB/PRS association was discovered for another repeating source of FRBs. However, it is not clear what makes FRBs or PRS or how they are related. We compile FRB and PRS properties to consider the population of FRB/PRS sources. We suggest a practical definition for PRS as FRB associations with luminosity greater than 10 29 erg s −1 Hz −1 that is not attributed to star-formation activity in the host galaxy. We model the probability distribution of the fraction of FRBs with PRS for repeaters and non-repeaters, showing there is not yet evidence for repeaters to be preferentially associated with PRS. We discuss how FRB/PRS sources may be distinguished by the combination of active repetition and an excess dispersion measure local to the FRB environment. We use CHIME/FRB event statistics to bound the mean per-source repetition rate of FRBs to be between 25 and 440 yr −1 . We use this to provide a bound on the density of FRB-emitting sources in the local universe of between 2.2 × 10 2 and 5.2 × 10 4 Gpc −3 assuming a pulsar-like beam width for FRB emission. This density implies that PRS may comprise as much as 1% of compact, luminous radio sources detected in the local universe. The cosmic density and phenomenology of PRS are similar to that of the newly-discovered, off-nuclear "wandering" AGN. We argue that it is likely that some PRS have already been detected and misidentified as AGN.

show abstract

“…Their origin from magnetars is preferred nowadays (Zhang 2020). FRBs take similarities to GPs (Lyu et al 2021) and can be viewed as super-GPs from young and rapidly spinning pulsars (Cordes & Wasserman 2016;Katz 2016;Lyutikov et al 2016). Previously, the authors Wang et al (2018) revealed evidence indicating that the repeating FRBs originate from starquake induced behaviour.…”

Section: Transient Phenomenamentioning

confidence: 99%

Transient phenomena from gas-erupting neutron stars

Li,

Wang

2021

Preprint

View full text Add to dashboard Cite

Starquakes probably occur in rapidly spinning or ultra high field neutron stars. In this short article, we argue that highly compressed gas containing electron-positron pairs could evaporate and erupt from inside the neutron star when a crack forms and then heals during a starquake. Under the influence of the existing oscillation modes of the star, the crack may have sufficiently large size and long lifetime. An appropriate amount of gas can erupt into the magnetosphere with relativistic and nearly uniform velocity, producing various transient and bursting phenomena.

show abstract

A comparison between repeating bursts of FRB 121102 and giant pulses from Crab pulsar and its applications

Cited by 21 publications

References 67 publications

Energy and waiting time distributions of FRB 121102 observed by FAST

Energy and waiting time distributions of FRB 121102 observed by FAST

On the Fast Radio Burst and Persistent Radio Source Populations

Transient phenomena from gas-erupting neutron stars

Contact Info

Product

Resources

About