A Wide-band High-frequency Type-II Solar Radio Burst

TL;DR

This paper reports a rare high-frequency, wide-band type-II solar radio burst originating from a dense streamer region, revealing detailed shock interactions and broad spectral features associated with CME shocks in the solar corona.

Contribution

It presents the first detailed observation of a high-frequency, wide-band type-II burst linked to CME-shock interaction with dense coronal loops, expanding understanding of solar radio emissions.

Findings

The burst's starting frequency reached 600-700 MHz.

The spectral bandwidth was as wide as ~300 MHz.

The source was associated with a shock dip near the solar surface.

Abstract

Type-II radio bursts are typically observed below ~ 400 MHz, with narrow-band slowly-drifting fundamental and harmonic structures. Here we report an unusual high-frequency wide-band type-II burst with starting frequency as high as 600 - 700 MHz and the instantaneous bandwidth being as wide as ~ 300 MHz. The estimated average spectral drift is ~ 2.18 MHz/s, its mean duration at each frequency is ~ 3 min, the maximum brightness temperature can exceed 10^11 to 10^12 K. According to the simultaneous EUV and radio imaging data, the radio sources distribute over a relatively broad region that concentrates around a dip of the nose front of the shock-like EUV wave structure. The dip is likely caused by the strong interaction of the eruption with the overlying closed dense loops that are enclosed by the large-scale streamer structure, indicating that the Type-II burst originates from such CME-shock interaction with dense-closed loop structures. The observations suggest that the unusual wide-band high frequency type-II radio burst originates from a dense streamer region in the corona, supported by EUV shock-like structure that get steepened very close to the solar surface ~ 1.23 R0 and type-II radio source coincides with the shock dip. Further the wide-band feature is due to the source stemming from a region with large density variation and not due to the intensity variation across the shock structure.