Journal ArticleDOI
Observations of Solar Type II bursts at frequencies 10–30 MHz
Valentin Melnik,A. A. Konovalenko,Helmut O. Rucker,Aleksander Stanislavsky,E. P. Abranin,Alain Lecacheux,G. Mann,A. Warmuth,V. V. Zaitsev,M. Y. Boudjada,V.V. Dorovskii,V. V. Zaharenko,V. N. Lisachenko,C. Rosolen +13 more
TLDR
In this paper, the results of radio telescope UTR-2 observations of solar Type II radio bursts in the 10-30-MHz frequency range are presented, which possess a fine structure consisting of fast drift sub-bursts similar to Type II bursts.Abstract:
We present the results of radio telescope UTR-2 observations of solar Type II radio bursts in the 10–30 MHz frequency range. These events possess a fine structure consisting of fast drift sub-bursts similar to Type III bursts. The frequency drift rate of the Type II bursts at decameter wavelengths is smaller than 0.1 MHz s−1. One of these bursts with herringbone structure has a wave-like backbone that almost does not drift. The features of the observed bursts are discussed.read more
Citations
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Journal ArticleDOI
Solar type ii radio bursts and ip type ii events
Hilary V. Cane,W. C. Erickson +1 more
TL;DR: In this paper, the authors examined radio data from the WAVES experiment on the Wind spacecraft in conjunction with ground-based data in order to investigate the relationship between the shocks responsible for metric type II radio bursts and the shocks in front of coronal mass ejections (CMEs).
Journal ArticleDOI
The influence of stellar wind conditions on the detectability of planetary radio emissions
TL;DR: In this paper, the authors compare the expected stellar and planetary radio signal for stellar systems of different ages, and show that conditions corresponding to the young solar system (i.e., with increased stellar wind density and velocity) appear to be more favorable than for older stellar systems.
Book ChapterDOI
Coherent Radio Emissions Associated with Solar System Shocks
TL;DR: A comprehensive review of the field can be found in this article, where the basic theory (electron shock acceleration, development of an electron beam, growth of Langmuir waves, and production of f pe and 2 f pe radiation for a macroscopic, rippled, shock) appears to explain the primary observations semiquantitatively, that many observational details and theoretical limitations remain unresolved, and that the next ten years ought to be an exciting time that sees theory and observations brought together quantitatively.
On Shock Wave Formation in the Solar Corona
TL;DR: In this article, Klassen et al. confirmed and extended earlier findings that type II bursts are emitted above active region loops seen in soft X-ray images, and they concluded that the type II burst is related to a plasma jet or a blast wave that originates in closed magnetic structures in the active region, and is first recognized during the early impulsive phase.
Journal ArticleDOI
An alternative to the plasma emission model: Particle-in-cell, self-consistent electromagnetic wave emission simulations of solar type III radio bursts
TL;DR: In this article, a superthermal, hot beam of electrons injected into a plasma thread that contains uniform longitudinal magnetic field and a parabolic density gradient was used to model electromagnetic wave emission generation in the context of solar type III radio bursts.
References
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Journal ArticleDOI
The Solar Corona in Active Regions and the Thermal Origin of the Slowly Varying Component of Solar Radio Radiation.
Journal ArticleDOI
On the association between type II radio bursts and CMEs
H. T. Claßen,H. Aurass +1 more
TL;DR: In this paper, the authors compared ground-based observations of metric (coronal) type II radio bursts with observations of coronal mass ejections (CMEs) obtained by the LASCO coronagraph aboard SOHO and with decametric (interplanetary) types of radio bursts recorded by the WAVES instrument aboard Wind.
Journal Article
A heliospheric density model and type III radio bursts
TL;DR: In this paper, a heliospheric density model is derived by evaluating the spherical solutions of magnetohydrostatic equations including the thermal pressure and the gravitational force of the Sun.