Clark Lake Radio Observations of Coronal Mass Ejections

1990 ◽  
pp. 495-500 ◽  
Author(s):  
N. Gopalswamy
Keyword(s):  
Coronal Mass Ejections ◽  
Radio Observations

Solar Radio Astronomy at Low Frequencies

2002 ◽  
Vol 199 ◽  
pp. 415-425
Author(s):  
Monique Pick
Keyword(s):  
Radio Telescope ◽  
Radio Astronomy ◽  
Coronal Mass Ejections ◽  
Solar Radio ◽  
Electron Beams ◽  
Solar Physics ◽  
Interplanetary Shocks ◽  
Radio Observations ◽  
Low Frequencies ◽  
Solar Radio Astronomy

This review is concerned to study of sun at frequencies lower than 1.4 GHz. Emphasis is made on results which illustrate the topics in which GMRT could play a major role. Coordinated studies including spectral and imaging radio observations are important for research in solar physics. Joint observations between the Giant Meter Radio Telescope (GMRT) with radio instruments located in the same longitude range are encouraged. This review inludes three distinct topics: Electron beams and radio observations- Radio signatures of Coronal Mass Ejections- Radio signatures of coronal and interplanetary shocks.

scholarly journals Clark Lake Radio Observations of Coronal Mass Ejections

1990 ◽  
Vol 142 ◽  
pp. 495-500
Author(s):  
N. Gopalswamy
Keyword(s):  
White Light ◽  
Coronal Mass Ejections ◽  
The Sun ◽  
Type Ii ◽  
Radio Observations ◽  
Magnetic Structures ◽  
Effect Relationship ◽  
Positional Analysis ◽  
Type Iv ◽  
Nonthermal Particles

We review some recent studies of mass ejections from the Sun using 2-D imaging observations of the Clark Lake multifrequency radioheliograph. Radio signatures of both fast and slow coronal mass ejections (CMEs) have been observed using the Clark Lake radioheliograph. Using temporal and positional analysis of moving type IV and type II bursts, and white light CMEs we find that the type II's and CMEs need not have a direct cause and effect relationship. Instead, the type II seems to be generated by a “decoupled shock”, probably due to an associated flare. The moving type IV burst requires nonthermal particles trapped in magnetic structures associated with the CME. Since nonthermal particles can be generated independent of the speed of CMEs, moving type IV bursts need not be associated only with fast CMEs. Specific examples are presented to support these views.

scholarly journals Radio Emission from the Sun and Stars: New Insights into Energetic Phenomena

2004 ◽  
Vol 219 ◽  
pp. 145-158
Author(s):  
T. S. Bastian
Keyword(s):  
Radio Emission ◽  
Energy Release ◽  
Coronal Mass Ejections ◽  
Magnetic Energy ◽  
Spectroscopic Techniques ◽  
The Sun ◽  
Late Type ◽  
Radio Observations ◽  
Dwarf Stars ◽  
Magnetic Energy Release

Energetic phenomena on the Sun and late-type stars pose a number of fascinating puzzles. These include coronal heating, flares, and coronal mass ejections, all believed to be manifestations of magnetic energy release. Radio radiation is a sensitive tracer of energetic phenomena on both the Sun and stars. Radio observations of the Sun over the past decade have produced new insights into the physics of magnetic energy release in flares and coronal mass ejections. Radio observations of late-type stars have exploited sensitive imaging and spectroscopic techniques to further constrain the nature of the relevant emission mechanisms. A surprise has been the recent discovery of radio emission from brown dwarf stars, implying the existence of substantial magnetic fields and a means of dissipating magnetic energy, neither of which are understood.

scholarly journals Radio and X-ray Investigations of Erupting Prominences

1998 ◽  
Vol 167 ◽  
pp. 358-365 ◽  
Author(s):  
N. Gopalswamy ◽  
Y. Hanaoka ◽  
J.R. Lemen
Keyword(s):  
Coronal Mass Ejections ◽  
Radio Observations ◽  
X Ray ◽  
Solar Disturbances ◽  
Simple Picture

AbstractProminence eruption is one of the most important solar phenomenon because of the possibility of using it as proxy of geoeffective solar disturbances. In a series of investigations using Nobeyama radio observations in conjunction with Yohkoh data we have found that there is more to a prominence eruption than the simple picture portrayed by Hα observations. The extent of coronal volume associated with the eruption is much larger than the prominence. We illustrate this with several examples and discuss the implication of the results for understanding the interplanetary manifestation of coronal mass ejections.

scholarly journals Radio Observations of Coronal Mass Ejections: Space Weather Aspects

2020 ◽  
Vol 7 ◽  
Author(s):  
Angelos Vourlidas ◽  
Eoin P. Carley ◽  
Nicole Vilmer
Keyword(s):  
Space Weather ◽  
Coronal Mass Ejections ◽  
Radio Observations

Solar radio observations and development of coronal mass ejections

2003 ◽  
Vol 32 (4) ◽  
pp. 467-472 ◽  
Author(s):  
M. Pick ◽  
D. Maia ◽  
Ch. Marqué
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Radio ◽  
Radio Observations

Coronal Mass Ejections and Solar Filament Disappearances at Solar Maximum

1994 ◽  
Vol 144 ◽  
pp. 127-129
Author(s):  
S. Dinulescu ◽  
G. Maris
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Maximum ◽  
Solar Filament

AbstractOccurrence of CMEs as a result of solar filament disappearance is discussed over the cycle 22.

White-Light Coronal Structures: Streamers and CMEs

1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
White Light ◽  
Coronal Mass Ejections ◽  
X Rays ◽  
Solar Cycles ◽  
Temperature Function ◽  
X Ray ◽  
Eclipse Observations ◽  
Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

Exploring Coronal Structures with SOHO

2000 ◽  
Vol 179 ◽  
pp. 403-406
Author(s):  
M. Karovska ◽  
B. Wood ◽  
J. Chen ◽  
J. Cook ◽  
R. Howard
Keyword(s):  
Solar Corona ◽  
Image Enhancement ◽  
Coronal Mass Ejections ◽  
Dynamical Evolution ◽  
Small Scale ◽  
Low Contrast ◽  
Contrast Structures ◽  
Scale Structures ◽  
Small Scale Structures ◽  
Coronal Structures

AbstractWe applied advanced image enhancement techniques to explore in detail the characteristics of the small-scale structures and/or the low contrast structures in several Coronal Mass Ejections (CMEs) observed by SOHO. We highlight here the results from our studies of the morphology and dynamical evolution of CME structures in the solar corona using two instruments on board SOHO: LASCO and EIT.

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