Role of photospheric footpoint shear in the impulsive dynamics of the solar corona

1996 ◽  
Vol 23 (21) ◽  
pp. 2955-2958 ◽  
Author(s):  
Z. W. Ma ◽  
A. Bhattacharjee
Keyword(s):  
Solar Corona ◽  
Impulsive Dynamics

Role of radio wave reflection during radio occultation by the solar corona

1985 ◽  
Vol 28 (7) ◽  
pp. 549-556 ◽  
Author(s):  
A. I. Kucheryavenkov ◽  
A. G. Pavel'ev ◽  
S. N. Rubtsov ◽  
O. I. Yakovlev
Keyword(s):  
Solar Corona ◽  
Radio Wave ◽  
Radio Occultation ◽  
Wave Reflection

The Role of Transient Brightenings in Heating the Solar Corona

2008 ◽  
Vol 689 (1) ◽  
pp. L77-L80 ◽  
Author(s):  
David H. Brooks ◽  
Ignacio Ugarte-Urra ◽  
Harry P. Warren
Keyword(s):  
Solar Corona

scholarly journals Mass and Energy Supply of Fine Structure to the Solar Corona

2004 ◽  
Vol 219 ◽  
pp. 123-127
Author(s):  
Kostas Tziotziou ◽  
Georgia Tsiropoula
Keyword(s):  
Solar Corona ◽  
Mass Balance ◽  
Magnetic Reconnection ◽  
Solar Atmosphere ◽  
Cloud Model ◽  
Physical Parameters ◽  
Mean Values ◽  
Fine Structures ◽  
Temporal And Spatial

We investigate the role of chromospheric fine structures, e.g. mottles (spicules), in the mass balance and heating of the solar atmosphere by studying two-dimensional high-resolution Hα observations. The temporal and spatial variations of the line-of-sight (LOS) velocity, obtained with an inversion technique based on a cloud model, provide strong indications that the mechanism responsible for the driving of the observed flows is magnetic reconnection. Apart from the LOS velocity, application of the cloud model enables the derivation of several other physical parameters, like pressure, temperature, density etc. Mean values of these parameters permit the estimation of the role of these structures in the mass balance of the solar atmosphere. They, furthermore, permit a reasonable estimate of the energy provided by magnetic reconnection which is available for the heating of the solar corona.

scholarly journals 66. Remarks on the energy of the nonthermal radio-frequency emission

1957 ◽  
Vol 4 ◽  
pp. 354-355
Author(s):  
L. Biermann ◽  
R. Lüst
Keyword(s):  
Radio Frequency ◽  
Solar Corona ◽  
Mechanical Energy ◽  
Acoustic Energy ◽  
Radiative Loss ◽  
Thermal Emissions ◽  
Outer Corona ◽  
Normal Feature ◽  
Frequency Emission

It is proposed to discuss the role of the radio-frequency emission in the whole set of the non-thermal emissions of the sun, which originate in the solar corona and the uppermost regions of the chromosphere. Of these, the radiative emissions give probably an amount of between 104and 105ergs/cm.2sec., to which the radio-frequency region contributes only very little (even during an intense outburst, when the total radiative emission is much larger, not more than 10°–102ergs/cm.2sec.); the contribution of the lower chromosphere, however, is not yet well known. The corpuscular emissions under normal conditions seem to require ≈ 105ergs/cm.2sec. (but again much more in active, e.g. ‘M’, regions), and to constitute a normal feature of the outer solar corona. These emissions, we propose, are maintained by the same supply of mechanical energy which secures the thermal and radiative equilibrium of the inner corona. That is to say, some part of the flux of acoustic energy originating in the hydrogen convection zone and, according to this theory, heating the upper chromosphere and the inner corona, is believed always to reach the outer corona, where the radiative loss is smaller, and this part is then at least comparable with that dissipated in the inner corona.*

scholarly journals ON THE ROLE OF REPETITIVE MAGNETIC RECONNECTIONS IN EVOLUTION OF MAGNETIC FLUX ROPES IN SOLAR CORONA

2016 ◽  
Vol 830 (2) ◽  
pp. 80 ◽  
Author(s):  
Sanjay Kumar ◽  
R. Bhattacharyya ◽  
Bhuwan Joshi ◽  
P. K. Smolarkiewicz
Keyword(s):  
Magnetic Flux ◽  
Solar Corona ◽  
Magnetic Flux Ropes ◽  
Flux Ropes

scholarly journals Storing free magnetic energy in the solar corona

2016 ◽  
Vol 82 (4) ◽  
Author(s):  
G. Vekstein
Keyword(s):  
Solar Corona ◽  
Solar Flares ◽  
Magnetic Energy ◽  
Solar Physics ◽  
Interested Reader ◽  
Convective Flows ◽  
Free Magnetic Energy ◽  
Wide Readership ◽  
Magnetic Arcade

This article presents a mini-tutorial aimed at a wide readership not familiar with the field of solar plasma physics. The exposition is centred around the issue of excess/free magnetic energy stored in the solar corona. A general consideration is followed with a particular example of coronal magnetic arcade, where free magnetic energy builds up by photospheric convective flows. In the context of solar physics the major task is to explain how this free energy can be released quickly enough to match what is observed in coronal explosive events such as solar flares. Therefore, in the last section of the paper we discuss briefly a possible role of magnetic reconnection in these processes. This is done in quite simple qualitative physical terms, so that an interested reader can follow it up in more detail with help of the provided references.

scholarly journals The Solar Corona

1980 ◽  
Vol 5 ◽  
pp. 335-341
Author(s):  
Claudio Chiuderi
Keyword(s):  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Structures

AbstractRecent observations from space have shown that the solar corona is spatially a very structured medium and temporally a very dynamic one. The consequent changes in the current theoretical ideas about coronal physics are reviewed. The role of the magnetic fields in shaping and heating the coronal structures is especially underlined.

Sign in / Sign up

Export Citation Format

Share Document