Long-duration non thermal energy release in flares and outside flares

A shock associated (SA) radio event and related phenomena observed from the base of the solar corona to 1 AU

“…This interpretation was challenged by some authors [Kundu et al, 1984[Kundu et al, , 1990Trotter, 1986;Klein, 1992;Klein and Trotter, 1994;Klein, 1995] who argued that, in many cases, the good correlation between the SA time profiles and the concurrent microwave burst and/or hard X-ray burst strongly suggested that the SA events were caused by electrons accelerated in or near the microwave or X-ray source region, i.e. near the chromosphere, rather than in coronal shock waves.…”

“…Some events appeared to be the extension of "herringbone structures" which are generally accepted to show evidence for shock acceleration [Nelson and Melrose, 1985;Cairns and Robinson, 1987]. In all cases, the radio signature began at distances larger than about 2 R(• from the sun center ( This interpretation was challenged by some authors [Kundu et al, 1984[Kundu et al, , 1990Trotter, 1986;Klein, 1992;Klein and Trotter, 1994;Klein, 1995] who argued that, in many cases, the good correlation between the SA time profiles and the concurrent microwave burst and/or hard X-ray burst strongly suggested that the SA events were caused by electrons accelerated in or near the microwave or X-ray source region, i.e. near the chromosphere, rather than in coronal shock waves.…”

Energetics of small electron acceleration episodes in the solar corona from radio noise storm observations

“…In this paper, we focus on radio noise storms, which are the archetypal example of electrons accelerated in small episodes outside of large flares (Klein 1995(Klein , 1998. This kind of emission is believed to be caused by accelerated electrons trapped in coronal arches above active regions.…”

Complex Type III‐like radio emissions observed from 1 to 14 MHz

“…Furthermore, Kahler et al [1986] found that about half of all metric type II bursts were associated with SA events for which there was no attributable metric type III, also in support of the Cane et al hypothesis. Further investigations of the time correlation between SA events and microwave and/or hard X-ray bursts suggested that SA events were produced by electrons accelerated low in the corona, rather than in large-scale coronal shocks [see Klein, 1995 …”

“…Furthermore, Kahler et al [1986] found that about half of all metric type II bursts were associated with SA events for which there was no attributable metric type III, also in support of the Cane et al hypothesis. Further investigations of the time correlation between SA events and microwave and/or hard X-ray bursts suggested that SA events were produced by electrons accelerated low in the corona, rather than in large-scale coronal shocks [see Klein, 1995 It is clear that the observations of SA events in the frequency range from 1 -14 MHz, i.e., in the gap between ground-based and space-based observation, is crucial for understanding the relationship between kilometric SA events and metric radio bursts, thereby providing important clues as to the origin and nature of SA events. This paper takes the first step by providing a morphological description of complex type IIIlike radio bursts observed from 1 -14 MHz, which corresponds to the transition region between the solar corona and interplanetary medium, i.e., from ~2 -10 R e A(Revee= heliocentric distance).…”