How Accurately Can We Determine the Coronal Heating Mechanism in the Large-Scale Solar Corona?

2001 ◽  
pp. 93-116
Author(s):  
D. H. Mackay ◽  
K. Galsgaard ◽  
E. R. Priest ◽  
C. R. Foley
Keyword(s):  
Solar Corona ◽  
Large Scale ◽  
Coronal Heating ◽  
Heating Mechanism

scholarly journals Coronal Heating Mechanism in the Presence of a Flow: A Numerical Approach

1998 ◽  
Vol 185 ◽  
pp. 469-470
Author(s):  
S. Parhi ◽  
T. Tanaka
Keyword(s):  
Magnetic Fields ◽  
Solar Corona ◽  
Plasma Heating ◽  
Inhomogeneous Plasma ◽  
Resonant Absorption ◽  
Numerical Approach ◽  
Coronal Heating ◽  
Heating Mechanism ◽  
Driving Current ◽  
Field Lines

The solar corona is a hot, tenuous plasma permeated with the structured magnetic fields. A variety of waves is generated in the corona due to the convective upwelling motion in the photosphere. The excitation of MHD fluctuations is generated by the footpoint motion of the field lines in the photosphere. Resonant absorption of the Alfvén waves in an inhomogeneous plasma has been suggested as a means of driving current and plasma heating in the corona (Sakurai et al., 1991). We study this problem in the presence of flow.

scholarly journals Propagation of an MHD Shock in the Vicinity of a Magnetic Neutral Sheet

1980 ◽  
Vol 91 ◽  
pp. 323-326
Author(s):  
D. J. Mullan ◽  
R. S. Steinolfson
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Solar Corona ◽  
Large Scale ◽  
Field Structure ◽  
Neutral Sheet ◽  
Solar Cosmic Rays ◽  
Magnetic Field Structure ◽  
Large Scale Magnetic Field ◽  
Highly Correlated

The acceleration of solar cosmic rays in association with certain solar flares is known to be highly correlated with the propagation of an MHD shock through the solar corona (Svestka, 1976). The spatial structure of the sources of solar cosmic rays will be determined by those regions of the corona which are accessible to the flare-induced shock. The regions to which the flare shock is permitted to propagate are determined by the large scale magnetic field structure in the corona. McIntosh (1972, 1979) has demonstrated that quiescent filaments form a single continuous feature (a “baseball stitch”) around the surface of the sun. It is known that helmet streamers overlie quiescent filaments (Pneuman, 1975), and these helmet streamers contain large magnetic neutral sheets which are oriented essentially radially. Hence the magnetic field structure in the low solar corona is characterized by a large-scale radial neutral sheet which weaves around the entire sun following the “baseball stitch”. There is therefore a high probability that as a shock propagates away from a flare, it will eventually encounter this large neutral sheet.

scholarly journals The Coronal Heating Mechanism as Identified by Full‐Sun Visualizations

2004 ◽  
Vol 615 (1) ◽  
pp. 512-525 ◽  
Author(s):  
Carolus J. Schrijver ◽  
Anne W. Sandman ◽  
Markus J. Aschwanden ◽  
Marc L. DeRosa
Keyword(s):  
Coronal Heating ◽  
Heating Mechanism

scholarly journals A contemporary view of coronal heating

2012 ◽  
Vol 370 (1970) ◽  
pp. 3217-3240 ◽  
Author(s):  
Clare E. Parnell ◽  
Ineke De Moortel
Keyword(s):  
Magnetic Field ◽  
Recent Progress ◽  
Coupled System ◽  
Coronal Heating ◽  
The Sun ◽  
Key Factors ◽  
Computing Power ◽  
Heating Mechanism ◽  
Outer Atmosphere ◽  
The Magnetic Field

Determining the heating mechanism (or mechanisms) that causes the outer atmosphere of the Sun, and many other stars, to reach temperatures orders of magnitude higher than their surface temperatures has long been a key problem. For decades, the problem has been known as the coronal heating problem, but it is now clear that ‘coronal heating’ cannot be treated or explained in isolation and that the heating of the whole solar atmosphere must be studied as a highly coupled system. The magnetic field of the star is known to play a key role, but, despite significant advancements in solar telescopes, computing power and much greater understanding of theoretical mechanisms, the question of which mechanism or mechanisms are the dominant supplier of energy to the chromosphere and corona is still open. Following substantial recent progress, we consider the most likely contenders and discuss the key factors that have made, and still make, determining the actual (coronal) heating mechanism (or mechanisms) so difficult.

OSO 8 observational limits to the acoustic coronal heating mechanism

1981 ◽  
Vol 247 ◽  
pp. 317 ◽  
Author(s):  
E. C., Jr. Bruner
Keyword(s):  
Coronal Heating ◽  
Heating Mechanism

The Large-Scale Density Structure of the Solar Corona and the Heliospheric Current Sheet

1996 ◽  
Vol 458 ◽  
pp. 817 ◽  
Author(s):  
Madhulika Guhathakurta ◽  
Thomas E. Holzer ◽  
R. M. MacQueen
Keyword(s):  
Solar Corona ◽  
Current Sheet ◽  
Large Scale ◽  
Heliospheric Current Sheet ◽  
Density Structure

scholarly journals Coronal global EIT waves as tools for multiple diagnostics

2007 ◽  
Vol 3 (S247) ◽  
pp. 243-250
Author(s):  
I. Ballai ◽  
M. Douglas
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Solar Disk ◽  
Coronal Loop ◽  
Large Scale ◽  
Theoretical Models ◽  
Coronal Loops ◽  
Quiet Sun ◽  
Propagating Waves ◽  
Global Magnetic Field

AbstractObservations in EUV lines of the solar corona revealed large scale propagating waves generated by eruptive events able to travel across the solar disk for large distances. In the low corona, CMEs are known to generate, e.g. EIT waves which can be used to sample the coronal local and global magnetic field. This contribution presents theoretical models for finding values of magnetic field in the quiet Sun and coronal loops based on the interaction of global waves and local coronal loops as well as results on the generation and propagation of EIT waves. The physical connection between local and global solar coronal events (e.g. flares, EIT waves and coronal loop oscillations) will also be explored.

Including the Transition Region in Models of the Large‐Scale Solar Corona

2001 ◽  
Vol 546 (1) ◽  
pp. 542-551 ◽  
Author(s):  
Roberto Lionello ◽  
Jon A. Linker ◽  
Zoran Mikić
Keyword(s):  
Solar Corona ◽  
Transition Region ◽  
Large Scale
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