Soft X-ray emissions, meter-wavelength radio bursts, and particle acceleration in solar flares

1988 ◽  
Vol 325 ◽  
pp. 895 ◽  
Author(s):  
H. V. Cane ◽  
D. V. Reames
Keyword(s):  
Particle Acceleration ◽  
Solar Flares ◽  
Radio Bursts ◽  
X Ray

Observations of Energetic Electrons in Solar Flares

1990 ◽  
Vol 142 ◽  
pp. 438-438
Author(s):  
B. Lokanadham
Keyword(s):  
Particle Acceleration ◽  
Energy Release ◽  
Observational Data ◽  
Solar Flares ◽  
Energetic Electrons ◽  
X Ray

A study of the simultaneous observations of solar flares in optical, radio and X-ray bands is important in understanding the process of energy release and particle acceleration in the explosive phenomena of solar flares. In order to determine the characteristics of such energetic electrons in solar flares, a total number of 50 two-ribbon flares have been carefully selected during the period 1979-89 having simultaneous observational data in the optical, X-ray and radio bands.

scholarly journals Radio and X-ray diagnostics of electrons accelerated in solar flares

2006 ◽  
Vol 2 (14) ◽  
pp. 88-88
Author(s):  
Miroslav Bárta ◽  
Marian Karlický
Keyword(s):  
Particle Acceleration ◽  
Solar Flare ◽  
Test Particle ◽  
Solar Flares ◽  
Global Scale ◽  
X Ray ◽  
Particle Simulations

AbstractStarting from 2.5D MHD modelling of solar flares on a global scale we calculate (using the PIC and test-particle simulations) the radio and X-ray emissions generated in solar flare reconnection. Our results – the radio and X-ray spectra and brightness distributions, and their dynamics – are directly comparable with observations providing thus a test of particle acceleration models as well as of the ‘standard’ global flare scenario.

Comparing different types of solar flares with radio bursts detected by SMOS

2020 ◽  
Author(s):  
Manuel Flores Soriano ◽  
Consuelo Cid
Keyword(s):  
Space Weather ◽  
Early Warning ◽  
Solar Flares ◽  
Solar Radio ◽  
The Sun ◽  
Radio Bursts ◽  
Radio Observatory ◽  
X Ray ◽  
Different Types ◽  
Mass Ejection

<p>SMOS is an Earth observing satellite that is been adapted to provide full polarization observations of the Sun at 1.4 GHz 24 hours a day. Its solar radio observations from the last decade will be released to the community by the middle of this year. In this presentation we show the capabilities of SMOS as a solar radio observatory and compare some of the most relevant radio bursts with data from GOES, LASCO, SDO and RSTN. We show how SMOS responds to different kinds of solar flares depending on their x-ray flux, and the kind of mass ejection or solar dimming that they have produced, if any. In addition to this we also show the potential of SMOS as a space weather tool to monitor GNSS satellites signal fades and to provide an early warning of Earth-directed coronal mass ejections.</p>

scholarly journals New Triggering Mechanism for Red Dwarf Flares

1983 ◽  
Vol 71 ◽  
pp. 609-611
Author(s):  
M.K. Das ◽  
J.N. Tandon
Keyword(s):  
Solar Flares ◽  
Galactic Cosmic Rays ◽  
Flare Activity ◽  
Radio Bursts ◽  
Triggering Mechanism ◽  
X Ray ◽  
Flare Stars ◽  
M Stars ◽  
Radio Band ◽  
Radio Flare

The flare phenomenon associated with dMe stars has received much attention in recent years (Gershberg 1975). Most of the flares have been detected in both optical and radio band (Lovell 1969; Kunkel 197U; Karpen et al, 1977). But as expected (Tandon 1976) only a few display weak soft X-ray emission (Karpen et al, 1977; Haisch and Linsky 1978)- Simultaneous X-ray, optical and radio observations of YZ CMi by Karpen et al (1977) shows no X-ray emission above 3σ level accompanying minor flares. Even coincident X-ray coverage with seven radio bursts shows no enhanced X-ray emission. Recently Haisch et al (1981) detected one well resolved X-ray flare on dM5e flare star Proxima Centauri and one coincident optical and radio flare out of five optical and twelve radio flare events. However, the X-ray flare on Proxima Centauri is not accompanied by any ultraviolet, optical or radio emission. Observations on flare stars show that they are more energetic, 102 - 103 times, than the corresponding solar flares. Considering the flare activity in dwarf M-stars to be similar but more energetic to that of a large solar flare, Tandon (1961) proposed red dwarf flares to be the source of low energy galactic cosmic rays. This hypothesis has been reexplored recently by Lovell (1974).

scholarly journals Plasma Processes in Solar Flares

1990 ◽  
Vol 142 ◽  
pp. 355-364
Author(s):  
V.M. Tomozov
Keyword(s):  
Solar Flares ◽  
Large Scale ◽  
Stark Effect ◽  
Active Regions ◽  
Theoretical Models ◽  
Radio Bursts ◽  
X Ray ◽  
Plasma Effects ◽  
Collective Plasma

A rationale is presented for a conception that appearance of flares in active regions is due to the interaction of large-scale convective elements. Such an interaction gives rise to shear motions in the vicinity of the inverse polarity line of the photospheric magnetic field which generate vortical motions leading to non-equilibrium state of the magnetic configuration. Modern concepts of manifestations of turbulent plasma processes are described in terms of theoretical models for solar flares. Plasma effects arising at propagation of electron beams and thermal fluxes in the solar atmosphere are considered. Their role in the interpretation of hard X-ray and type III radio bursts is pointed out. The role of the turbulent Stark effect for diagnostics of collective plasma processes in solar flares is emphasized.

scholarly journals Particle Acceleration in Solar Flares

1974 ◽  
Vol 57 ◽  
pp. 437-445 ◽  
Author(s):  
P. A. Sturrock
Keyword(s):  
Particle Acceleration ◽  
Field Line ◽  
Solar Flares ◽  
Phase 1 ◽  
Turbulent Plasma ◽  
Radio Bursts ◽  
Type Ii ◽  
Phase 2 ◽  
Type Iv ◽  
Magnetohydrodynamic Shock

A review of observational data supports the proposal that there are two distinct phases of particle acceleration in solar flares. ‘Phase 1’ is associated with the flash phase and is here interpreted as acceleration during field-line reconnection. ‘Phase 2’ is associated with type II and type IV radio bursts, and is ascribed to stochastic acceleration in the turbulent plasma behind a magnetohydrodynamic shock formed ahead of an ejected plasmoid.

scholarly journals Analysis of some solar flares from optical, X-ray, and radio observations

1968 ◽  
Vol 35 ◽  
pp. 449-464
Author(s):  
R. Falciani ◽  
M. Landini ◽  
A. Righini ◽  
M. Rigutti
Keyword(s):  
Solar Flares ◽  
High Intensity ◽  
Radio Bursts ◽  
X Rays ◽  
Radio Observations ◽  
X Ray ◽  
Optical Flare

Using an improved isodensitometric technique it has been possible to study in great detail the photometric structure and the evolution of eight flares. A comparison has been made between the evolutive curves and the ones obtained from measurements of solar X-rays and radio fluxes at λλ 3·2 and 21 cm.A reduction of the flare areas (and of the emitted energies) before the flash phase and a continuous pulsation of the flare have been observed. Further it seems that the flares associated with radio bursts or X-ray events are those which show regions of a sufficiently high intensity, the emitting areas not being a very important parameter.The correlation in time between the various examined aspects of the AR seems to indicate that the sequence for the beginning of the different phenomena is, in general: optical flare, X-ray events, radio events.

Particle acceleration and the decay of soft X-ray non-thermal line broadening in solar flares

Solar Physics ◽  
1994 ◽  
Vol 154 (1) ◽  
pp. 157-175 ◽  
Author(s):  
David Alexander ◽  
Sarah A. Matthews
Keyword(s):  
Particle Acceleration ◽  
Solar Flares ◽  
Line Broadening ◽  
X Ray ◽  
Thermal Line

Statistical study of the correlation of hard X-ray and type III radio bursts in solar flares

1990 ◽  
Vol 358 ◽  
pp. 644 ◽  
Author(s):  
Russell J. Hamilton ◽  
Vahe Petrosian ◽  
A. O. Benz
Keyword(s):  
Solar Flares ◽  
Statistical Study ◽  
Radio Bursts ◽  
X Ray ◽  
Type Iii
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