scholarly journals Evaluation of solar Type II radio burst estimates of initial solar wind shock speed using a kinematic model of the solar wind on the April 2001 solar event swarm

2002 ◽  
Vol 29 (8) ◽  
pp. 12-1-12-4 ◽  
Author(s):  
W. Sun ◽  
M. Dryer ◽  
C. D. Fry ◽  
C. S. Deehr ◽  
Z. Smith ◽  
...  
Keyword(s):  
Solar Wind ◽  
Radio Burst ◽  
Kinematic Model ◽  
Type Ii ◽  
Solar Event ◽  
Shock Speed ◽  
Solar Type

Kinetic Simulations of Solar Type II Radio Burst Emission Processes

2010 ◽  
Author(s):  
Urs Ganse ◽  
Thomas Burkart ◽  
Felix Spanier ◽  
Rami Vainio ◽  
M. Maksimovic ◽  
...  
Keyword(s):  
Radio Burst ◽  
Type Ii ◽  
Solar Type ◽  
Burst Emission

scholarly journals A BROKEN SOLAR TYPE II RADIO BURST INDUCED BY A CORONAL SHOCK PROPAGATING ACROSS THE STREAMER BOUNDARY

2012 ◽  
Vol 750 (2) ◽  
pp. 158 ◽  
Author(s):  
X. L. Kong ◽  
Y. Chen ◽  
G. Li ◽  
S. W. Feng ◽  
H. Q. Song ◽  
...  
Keyword(s):  
Radio Burst ◽  
Type Ii ◽  
Coronal Shock ◽  
Solar Type

Fine Structure of a Solar Type II Radio Burst Observed by LOFAR

2020 ◽  
Vol 897 (1) ◽  
pp. L15
Author(s):  
Jasmina Magdalenić ◽  
Christophe Marqué ◽  
Richard A. Fallows ◽  
Gottfried Mann ◽  
Christian Vocks ◽  
...  
Keyword(s):  
Fine Structure ◽  
Radio Burst ◽  
Type Ii ◽  
Solar Type

scholarly journals A SOLAR TYPE II RADIO BURST FROM CORONAL MASS EJECTION-CORONAL RAY INTERACTION: SIMULTANEOUS RADIO AND EXTREME ULTRAVIOLET IMAGING

2014 ◽  
Vol 787 (1) ◽  
pp. 59 ◽  
Author(s):  
Yao Chen ◽  
Guohui Du ◽  
Li Feng ◽  
Shiwei Feng ◽  
Xiangliang Kong ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Radio Burst ◽  
Extreme Ultraviolet ◽  
Type Ii ◽  
Solar Type ◽  
Mass Ejection

TEMPORAL SPECTRAL SHIFT AND POLARIZATION OF A BAND-SPLITTING SOLAR TYPE II RADIO BURST

2014 ◽  
Vol 793 (2) ◽  
pp. L39 ◽  
Author(s):  
Guohui Du ◽  
Yao Chen ◽  
Maoshui Lv ◽  
Xiangliang Kong ◽  
Shiwei Feng ◽  
...  
Keyword(s):  
Radio Burst ◽  
Spectral Shift ◽  
Type Ii ◽  
Band Splitting ◽  
Solar Type

scholarly journals Shock Location and CME 3-D Reconstruction of a Solar Type II Radio Burst with LOFAR

2018 ◽  
Author(s):  
Pietro Zucca ◽  
Diana E. Morosan ◽  
Alexis Rouillard ◽  
Richard Fallows ◽  
Peter T. Gallagher ◽  
...  
Keyword(s):  
Radio Burst ◽  
Type Ii ◽  
Solar Type ◽  
Shock Location

scholarly journals Progress on Coronal, Interplanetary, Foreshock, and Outer Heliospheric Radio Emissions

2000 ◽  
Vol 17 (1) ◽  
pp. 22-34 ◽  
Author(s):  
Iver H. Cairns ◽  
P. A. Robinson ◽  
G. P. Zank
Keyword(s):  
Solar Wind ◽  
Plasma Waves ◽  
Recent Theory ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Radio Emissions ◽  
Source Regions ◽  
Earth’S Bow Shock ◽  
Made In

AbstractType II and III solar radio bursts are associated with shock waves and streams of energetic electrons, respectively, which drive plasma waves and radio emission at multiples of the electron plasma frequency as they move out from the corona into the interplanetary medium. Analogous plasma waves and radiation are observed from the foreshock region upstream of Earth's bow shock. In situ spacecraft observations in the solar wind have enabled major progress to be made in developing quantitative theories for these phenomena that are consistent with available data. Similar processes are believed responsible for radio emissions at 2–3 kHz that originate in the distant heliosphere, from where the solar wind interacts with the local interstellar medium. The primary goal of this paper is to review the observations and theories for these four classes of emissions, focusing on recent progress in developing detailed theories for the plasma waves and radiation in the source regions. The secondary goal is to introduce and review stochastic growth theory, a recent theory which appears quantitatively able to explain the wave observations in type III bursts and Earth's foreshock and is a natural theory to apply to type II bursts, the outer heliospheric emissions, and perhaps astrophysicalemissions.

scholarly journals Analyzing the propagation of EUV waves and their connection with type II radio bursts by combining numerical simulations and multi-instrument observations

2020 ◽  
Vol 644 ◽  
pp. A90
Author(s):  
A. Koukras ◽  
C. Marqué ◽  
C. Downs ◽  
L. Dolla
Keyword(s):  
Magnetic Field ◽  
Wave Front ◽  
Ray Tracing ◽  
Radio Burst ◽  
Radio Bursts ◽  
Type Ii ◽  
Fast Mode ◽  
Type Ii Radio Bursts ◽  
The Magnetic Field ◽  
Burst Emission

Context. EUV (EIT) waves are wavelike disturbances of enhanced extreme ultraviolet (EUV) emission that propagate away from an eruptive active region across the solar disk. Recent years have seen much debate over their nature, with three main interpretations: the fast-mode magneto-hydrodynamic (MHD) wave, the apparent wave (reconfiguration of the magnetic field), and the hybrid wave (combination of the previous two). Aims. By studying the kinematics of EUV waves and their connection with type II radio bursts, we aim to examine the capability of the fast-mode interpretation to explain the observations, and to constrain the source locations of the type II radio burst emission. Methods. We propagate a fast-mode MHD wave numerically using a ray-tracing method and the WKB (Wentzel-Kramers-Brillouin) approximation. The wave is propagated in a static corona output by a global 3D MHD Coronal Model, which provides density, temperature, and Alfvén speed in the undisturbed coronal medium (before the eruption). We then compare the propagation of the computed wave front with the observed wave in EUV images (PROBA2/SWAP, SDO/AIA). Lastly, we use the frequency drift of the type II radio bursts to track the propagating shock wave, compare it with the simulated wave front at the same instant, and identify the wave vectors that best match the plasma density deduced from the radio emission. We apply this methodology for two EUV waves observed during SOL2017-04-03T14:20:00 and SOL2017-09-12T07:25:00. Results. The simulated wave front displays a good qualitative match with the observations for both events. Type II radio burst emission sources are tracked on the wave front all along its propagation. The wave vectors at the ray-path points that are characterized as sources of the type II radio burst emission are quasi-perpendicular to the magnetic field. Conclusions. We show that a simple ray-tracing model of the EUV wave is able to reproduce the observations and to provide insight into the physics of such waves. We provide supporting evidence that they are likely fast-mode MHD waves. We also narrow down the source region of the radio burst emission and show that different parts of the wave front are responsible for the type II radio burst emission at different times of the eruptive event.

scholarly journals Source Region of the Decameter–Hectometric Type II Radio Burst: Shock–Streamer Interaction Region

Solar Physics ◽  
2012 ◽  
Vol 282 (2) ◽  
pp. 543-552 ◽  
Author(s):  
Chenglong Shen ◽  
Chijian Liao ◽  
Yuming Wang ◽  
Pinzhong Ye ◽  
Shui Wang
Keyword(s):  
Radio Burst ◽  
Source Region ◽  
Interaction Region ◽  
Type Ii
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