Fine Structures of Solar Radio Type III Bursts and Their Possible Relationship with Coronal Density Turbulence

Xingyao Chen, Eduard P. Kontar, Sijie Yu, Yihua Yan, Jing Huang, Baolin Tan

Research output: Contribution to journalArticlepeer-review

14 Scopus citations

Abstract

Solar radio type III bursts are believed to be the most sensitive signatures of near-relativistic electron beam propagation in the corona. A solar radio type IIIb-III pair burst with fine frequency structures, observed by the Low Frequency Array (LOFAR) with high temporal (∼10 ms) and spectral (12.5 kHz) resolutions at 30-80 MHz, is presented. The observations show that the type III burst consists of many striae, which have a frequency scale of about 0.1 MHz in both the fundamental (plasma) and the harmonic (double plasma) emission. We investigate the effects of background density fluctuations based on the observation of striae structure to estimate the density perturbation in the solar corona. It is found that the spectral index of the density fluctuation spectrum is about -1.7, and the characteristic spatial scale of the density perturbation is around 700 km. This spectral index is very close to a Kolmogorov turbulence spectral index of -5/3, consistent with a turbulent cascade. This fact indicates that the coronal turbulence may play the important role of modulating the time structures of solar radio type III bursts, and the fine structure of radio type III bursts could provide a useful and unique tool to diagnose the turbulence in the solar corona.

Original languageEnglish (US)
Article number73
JournalAstrophysical Journal
Volume856
Issue number1
DOIs
StatePublished - Mar 20 2018

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Sun: corona
  • Sun: radio radiation
  • solar wind

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