Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154

  title={Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154},
  author={D Simard and Vikram Ravi},
  journal={The Astrophysical Journal Letters},
  • D. Simard, V. Ravi
  • Published 23 June 2020
  • Physics
  • The Astrophysical Journal Letters
The discovery of a fast radio burst (FRB) associated with a magnetar in the Milky Way by the Canadian Hydrogen Intensity Mapping Experiment FRB collaboration (CHIME/FRB) and the Survey for Transient Astronomical Radio Emission 2 has provided an unprecedented opportunity to refine FRB emission models. The burst discovered by CHIME/FRB shows two components with different spectra. We explore interstellar scintillation as the origin for this variation in spectral structure. Modeling a weak… 

Figures and Tables from this paper

Fast Radio Bursts
The era of fast radio bursts (FRBs) was open in 2007, when a very bright radio pulse of unknown origin was discovered occasionally in the archival data of Parkes Telescope. Over the past fifteen
Magnetospheric Curvature Radiation by Bunches as Emission Mechanism for Repeating Fast Radio Bursts
Coherent curvature radiation as the radiation mechanism for fast radio bursts (FRBs) has been discussed since FRBs were discovered. We study the spectral and polarization properties of repeating
A Toy Model for the Time–Frequency Structure of Fast Radio Bursts: Implications for the CHIME/FRB Burst Dichotomy
We introduce a toy model for the time–frequency structure of fast radio bursts, in which the observed emission is produced as a narrowly peaked intrinsic spectral energy distribution sweeps down in
Observational Effects of Banded Repeating FRBs
  • K. Aggarwal
  • Physics
    The Astrophysical Journal Letters
  • 2021
Recent observations have shown that repeating fast radio bursts (FRBs) exhibit band-limited emission, whose frequency-dependent amplitude can be modeled using a Gaussian function. In this analysis,
An analysis of the time-frequency structure of several bursts from FRB 121102 detected with MeerKAT
We present a detailed study of the complex time-frequency structure of a sample of previously reported bursts of FRB 121102 detected with the MeerKAT telescope in September 2019. The wide
The Thousand-Pulsar-Array programme on MeerKAT – III. Giant pulse characteristics of PSR J0540−6919
PSR J0540–6919 is the second-most energetic radio pulsar known and resides in the Large Magellanic Cloud. Like the Crab pulsar it is observed to emit giant radio pulses (GPs). We used the
The physics of fast radio bursts
In 2007, a very bright radio pulse was identified in the archival data of the Parkes Telescope in Australia, marking the beginning of a new research branch in astrophysics. In 2013, this kind of
Constraining Galaxy Halos from the Dispersion and Scattering of Fast Radio Bursts and Pulsars
Fast radio bursts (FRBs) can be scattered by ionized gas in their local environments, host galaxies, intervening galaxies along their lines of sight (LOS), the intergalactic medium, and the Milky
Evidence of a shared spectro-temporal law between sources of repeating fast radio bursts
We study the spectro-temporal characteristics of two repeating fast radio bursts (FRBs), namely, FRB 20180916B and FRB 20180814A , and combine the results with those from our earlier analysis on
Detection of two bright radio bursts from magnetar SGR 1935 + 2154
Fast radio bursts (FRBs) are millisecond-duration, bright radio signals (fluence $\mathrm{0.1 - 100\,Jy\,ms}$) emitted from extragalactic sources of unknown physical origin. The recent CHIME/FRB and


High time resolution and polarization properties of ASKAP-localized fast radio bursts
Combining high time and frequency resolution full-polarisation spectra of Fast Radio Bursts (FRBs) with knowledge of their host galaxy properties provides an opportunity to study both the emission
A unified picture of Galactic and cosmological fast radio bursts
The discovery of a fast radio burst (FRB) in our galaxy associated with a magnetar (neutron star with strong magnetic field) has provided a critical piece of information to help us finally understand
A fast radio burst associated with a Galactic magnetar.
The discovery of FRB 200428 implies that active magnetars such as SGR 1935+2154 can produce FRBs at extragalactic distances, and favours emission models that describe synchrotron masers or electromagnetic pulses powered by magnetar bursts and giant flares.
Implications of a Fast Radio Burst from a Galactic Magnetar
A luminous radio burst was recently detected in temporal coincidence with a hard X-ray flare from the Galactic magnetar SGR 1935+2154 with a time and frequency structure consistent with cosmological
Constraints on the engines of fast radio bursts
We model the sample of fast radio bursts (FRBs), including the newly discovered CHIME repeaters, using the decelerating synchrotron maser blast wave model of Metzger, Margalit & Sironi (2019),
Dense magnetized plasma associated with a fast radio burst
The examination of archival data revealing Faraday rotation in the fast radio burst FRB 110523 is reported, indicating magnetization in the vicinity of the source itself or within a host galaxy.
Insight-HXMT X-ray and hard X-ray detection of the double peaks of the Fast Radio Burst from SGR 1935+2154
Here we report a refined analysis of the Insight-HXMT light curves, which have been corrected for data saturation and dead-time effects. Insight-HXMT light curves could be found at:
Plasmoid Ejection by Alfvén Waves and the Fast Radio Bursts from SGR 1935+2154
Using numerical simulations we show that low-amplitude Alfvén waves from a magnetar quake propagate to the outer magnetosphere and convert to “plasmoids” (closed magnetic loops) that accelerate from
A census of baryons in the Universe from localized fast radio bursts
The baryon density determined along the lines of sight to localized fast radio bursts is consistent with that determined from the cosmic microwave background and required by Big Bang nucleosynthesis.