Theory of type III and type II solar radio emissions

2000 ◽  
pp. 37-45 ◽  
Author(s):  
P. A. Robinson ◽  
I. H. Cairns
Keyword(s):  
Solar Radio ◽  
Type Ii ◽  
Radio Emissions ◽  
Type Iii ◽  
Solar Radio Emissions

scholarly journals Nonlinear analysis of decimetric solar bursts

2009 ◽  
Vol 5 (S264) ◽  
pp. 279-281
Author(s):  
Reinaldo R. Rosa ◽  
Mauricio J. A. Bolzan ◽  
Francisco C. R. Fernandes ◽  
H. S. Sawant ◽  
Marian Karlický
Keyword(s):  
Solar Radio ◽  
Inhomogeneous Plasma ◽  
Active Regions ◽  
Singularity Spectrum ◽  
Frequency Range ◽  
Radio Emissions ◽  
Magnetic Structures ◽  
Fine Structures ◽  
Solar Bursts ◽  
Solar Radio Emissions

AbstractThe solar radio emissions in the decimetric frequency range (above 1 GHz) are very rich in temporal and spectral fine structures due to nonlinear processes occurring in the magnetic structures on the corresponding active regions. In this paper we characterize the singularity spectrum, f(α), for solar bursts observed at 1.6, 2.0 and 3 GHz. We interpret our findings as evidence of inhomogeneous plasma turbulence driving the underlying plasma emission process and discuss the nonlinear multifractal approach into the context of geoeffective solar active regions.

scholarly journals Recent Results of Meter-decameter Wave Observations of Solar Flares

1989 ◽  
Vol 104 (2) ◽  
pp. 185-189
Author(s):  
N. Copalswamy ◽  
M. R. Kundu
Keyword(s):  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Type Iv

AbstractWe present recent results from meter-decameter imaging of several classes of solar radio bursts: Preflare activity in the form of type III bursts, correlated type IIIs from distant sources, and type II and moving type IV bursts associated with flares and CMEs.

scholarly journals Numerical Simulation of Type III Bursts

1980 ◽  
Vol 86 ◽  
pp. 299-302
Author(s):  
T. Takakura
Keyword(s):  
Numerical Simulation ◽  
Analytical Method ◽  
Solar Radio ◽  
Plasma Waves ◽  
Radio Bursts ◽  
Emission Mechanism ◽  
Normal Type ◽  
Solar Radio Bursts ◽  
Radio Emissions ◽  
Type Iii

By the use of semi-analytical method, modeling of three kinds of type III solar radio bursts have been made. Many basic problems about the type III bursts and associated solar electrons have been solved showing some striking or unexpected results. If the fundamental radio emissions should be really observed as the normal type III bursts, the emission mechanism would not be the currently accepted one, i.e. the scattering of plasma waves by ions.

Solar radio emissions

2005 ◽  
Vol 35 (5) ◽  
pp. 739-754 ◽  
Author(s):  
J.-P. Raulin ◽  
A.A. Pacini
Keyword(s):  
Solar Radio ◽  
Radio Emissions ◽  
Solar Radio Emissions

Solar Radio Emissions and Sunspots

Nature ◽  
1948 ◽  
Vol 161 (4082) ◽  
pp. 134-136 ◽  
Author(s):  
I. L. THOMSEN
Keyword(s):  
Solar Radio ◽  
Radio Emissions ◽  
Solar Radio Emissions

scholarly journals Effects of Solar Radio Emissions on Outdoor Propagation Path Loss Models at 60 GHz Bands for Access/Backhaul Links and D2D Communications

2017 ◽  
Vol 65 (12) ◽  
pp. 6624-6635 ◽  
Author(s):  
Ahmed Iyanda Sulyman ◽  
Hussein Seleem ◽  
Abdulmalik Alwarafy ◽  
Khaled M. Humadi ◽  
Abdulhameed Alsanie
Keyword(s):  
Solar Radio ◽  
Path Loss ◽  
Propagation Path ◽  
60 Ghz ◽  
D2d Communications ◽  
Radio Emissions ◽  
Loss Models ◽  
Solar Radio Emissions ◽  
Backhaul Links

scholarly journals Type II Solar Radio Burst with a Split and Herring − Bones during a Minimum Solar Activity

2014 ◽  
Vol 32 ◽  
pp. 104-111
Author(s):  
Zety Sharizat Hamidi ◽  
N.N.M. Shariff ◽  
C. Monstein
Keyword(s):  
Solar Activity ◽  
Solar Flare ◽  
Radio Burst ◽  
Solar Flares ◽  
Solar Radio ◽  
Correlation Study ◽  
Solar Radio Burst ◽  
Type Ii ◽  
Type Iii ◽  
Lower Stage

A preliminary correlation study of the herring − bone type II with a type III solar burst of has been made. On the basis of this study and in combination with the observation in radio emission, an interpretation of the mechanism of the occurrence of this event has been proposed. The type II solar radio burst with a split and herring bone is occurring at the same time from 36 MHz till 50 MHz. We have noted that an individual type III burst also can be observed at 13:23 UT from 45-50 MHz. During that day, a stream of solar wind from a coronal hole on the Sun has disturbing Earth's magnetosphere creating a minor geomagnetic storm, G1 on the NOAA scale of G1-G5. In this case, the solar flare is not very high, but CME is responsible to form a solar radio burst type II. Overall, based on seven days observation beginning from 25th March 2013, the solar activity is considered as very low. The highest solar flare can be observed within 7 days is only a class of B8 flare. There was no CMEs event that directed to the Earth is detected. The geomagnetic field activities are also at minimum level. Although the solar flare event is at a lower stage, it is still possible to form the solar radio burst type II which is associated with CME event. From the selected event, although theoretically solar radio burst type II is associated with CMEs, there is no compelling solar radio burst type II without a flare. The only difference is the dynamic structure and the intensity and speed of both phenomena (solar flares and CMEs) which depend on the active region. Nevertheless, understanding how energy is released in solar flares is one of the central questions in astrophysics. This solar radio burst type II formation is the first event that successfully detected by e-CALLISTO network in 2013.

The Positions of Associated Type II and Type III Solar Radio Bursts

1974 ◽  
Vol 2 (5) ◽  
pp. 255-258 ◽  
Author(s):  
R. A. Duncan
Keyword(s):  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Intense Burst ◽  
Lower Frequencies

Large solar radio outbursts at metre wavelengths often consist of a group of type III bursts followed a few minutes later by a type II burst; in both spectral types the intense burst radiation drifts towards lower frequencies with time (Figure 1).

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