Periodicities in an active region correlated with Type III radio bursts observed by Parker Solar Probe

TL;DR

This study finds that ~5-minute periodicities in EUV emissions and Type III radio bursts are correlated in an active solar region, indicating periodic non-thermal electron acceleration likely linked to small impulsive events like nanoflares.

Contribution

It demonstrates a correlation between EUV periodicities and Type III radio bursts without large flares, suggesting a new link between small impulsive events and electron acceleration in the corona.

Findings

Periodicities of about 5 minutes in EUV are correlated with Type III burst repetition rates.

EUV light curves show impulsive heating and cooling cycles in the active region.

Evidence of microflares and nanoflares associated with electron acceleration, without large flares.

Abstract

Context. Periodicities have frequently been reported across many wavelengths in the solar corona. Correlated periods of ~5 minutes, comparable to solar p-modes, are suggestive of coupling between the photosphere and the corona. Aims. Our study investigates whether there are correlations in the periodic behavior of Type III radio bursts, indicative of non-thermal electron acceleration processes, and coronal EUV emission, assessing heating and cooling, in an active region when there are no large flares. Methods. We use coordinated observations of Type III radio bursts from the FIELDS instrument on Parker Solar Probe (PSP), of extreme ultraviolet emissions by the Solar Dynamics Observatory (SDO)/AIA and white light observations by SDO/HMI, and of solar flare x-rays by Nuclear Spectroscopic Telescope Array (NuSTAR) on April 12, 2019. Several methods for assessing periodicities are utilized and compared to validate periods obtained. Results. Periodicities of about 5 minutes in the EUV in several areas of an active region are well correlated with the repetition rate of the Type III radio bursts observed on both PSP and Wind. Detrended 211A and 171A light curves show periodic profiles in multiple locations, with 171A peaks lagging those seen in 211A. This is suggestive of impulsive events that result in heating and then cooling in the lower corona. NuSTAR x-rays provide evidence for at least one microflare during the interval of Type III bursts, but there is not a one-to-one correspondence between the x-rays and the Type-III bursts. Our study provides evidence for periodic acceleration of non-thermal electrons (required to generate Type III radio bursts) when there were no observable flares either in the x-ray data or the EUV. The acceleration process, therefore, must be associated with small impulsive events, perhaps nanoflares.