Io-Jupiter Electrodynamic Interaction, Electron Acceleration and Radio Bursts Generation (abstract)

Electron acceleration at quasi-parallel shocks in the solar corona and its signature in solar Type II radio bursts

The Astrophysical Journal Supplement Series ◽

10.1086/191877 ◽

1994 ◽

Vol 90 ◽

pp. 577 ◽

Cited By ~ 10

Author(s):

G. Mann ◽

H. Luehr

Keyword(s):

Solar Corona ◽

Electron Acceleration ◽

Radio Bursts ◽

Type Ii ◽

Type Ii Radio Bursts ◽

Solar Type

Download Full-text

Efficiency of electron acceleration by shock waves in the solar corona according to observational data on the fine structure of type II radio bursts

Radiophysics and Quantum Electronics ◽

10.1007/bf02679627 ◽

1998 ◽

Vol 41 (2) ◽

pp. 107-114 ◽

Cited By ~ 1

Author(s):

V. V. Zaitsev ◽

E. Y. Zlotnik ◽

G. Mann ◽

H. Aurass ◽

A. Klassen

Keyword(s):

Fine Structure ◽

Shock Waves ◽

Solar Corona ◽

Observational Data ◽

Electron Acceleration ◽

Radio Bursts ◽

Type Ii ◽

Type Ii Radio Bursts

Download Full-text

The nature and origin of moving solar radio bursts associated with coronal mass ejections

10.5194/egusphere-egu2020-5379 ◽

2020 ◽

Author(s):

Diana Morosan ◽

Emilia Kilpua ◽

Erika Palmerio ◽

Benjamin Lynch ◽

Jens Pomoell ◽

...

Keyword(s):

Coronal Mass Ejections ◽

Magnetic Energy ◽

Direct Methods ◽

Electron Acceleration ◽

Three Dimensions ◽

The Sun ◽

Radio Bursts ◽

Type Ii ◽

Type Iv ◽

Multi Wavelength

Flares and coronal mass ejections (CMEs) from the Sun are the most powerful and spectacular explosions in the solar system, capable of releasing vast amounts of magnetic energy over relatively short periods of time. These phenomena are often associated with particle acceleration processes that are often observed directly by spacecraft here at Earth. At the Sun, there are no direct methods of measuring these particles, which is necessary to predict their origin and propagation direction through the heliosphere. However, accelerated particles, in particular fast electrons, can generate emission at radio wavelengths through various mechanisms. Here, we exploit radio observations of Type II and Type IV radio bursts that accompany CME eruptions, in particular those radio bursts that show movement with the CME expansion in the low solar corona. Using multi-wavelength analysis, reconstruction of the radio emission and CME in three dimensions, we aim to determine the sources and locations of electron acceleration responsible for the Type II and Type IV emission in relation to the CME location and propagation. Such studies are important to&#160;understand CMEs and the sources of electron acceleration to ultimately improve the lead time to these impacts here at Earth.

Download Full-text

Type II Solar Radio Bursts over Solar Cycle 21

International Astronomical Union Colloquium ◽

10.1017/s025292110002546x ◽

1994 ◽

Vol 144 ◽

pp. 283-284

Author(s):

G. Maris ◽

E. Tifrea

Keyword(s):

Solar Radio ◽

Interplanetary Space ◽

Impulsive Phase ◽

Radio Bursts ◽

Type Ii ◽

Solar Radio Bursts ◽

Strong Energy ◽

Mass Ejection ◽

Geophysical Effect ◽

Radio Event

The type II solar radio bursts produced by a shock wave passing through the solar corona are one of the most frequently studied solar activity phenomena. The scientific interest in this type of phenomenon is due to the fact that the presence of this radio event in a solar flare is an almost certain indicator of a future geophysical effect. The origin of the shock waves which produce these bursts is not at all simple; besides the shocks which are generated as a result of a strong energy release during the impulsive phase of a flare, there are also the shocks generated by a coronal mass ejection or the shocks which appear in the interplanetary space due to the supplementary acceleration of the solar particles.

Download Full-text