Volume 455, Number 3, September I 2006
|Page(s)||1115 - 1121|
|Published online||16 August 2006|
Heating the solar corona by plasma loops
Mathematical Institute, University of Oxford, 24–29 St Giles', Oxford OX1 3LB, UK e-mail: email@example.com;firstname.lastname@example.org
Accepted: 23 May 2006
We investigate the heating of the corona via plasma loops. It is shown that it may be possible to maintain the high corona temperatures using plasma loops as conduits. Under certain conditions heat can flow across magnetic fields up temperature gradients, a mechanism that has been previously applied to the heating of plasma loops. A typical conduit loop is hotter than the ambient plasma in the upper chromosphere and transition layer, and is cooler than the ambient plasma in the background corona. Hence, heat enters the loop at the bottom, is transported by a combination of conduction (if there is a negative temperature gradient), convection and shock waves up the loop into the corona. Typical values show that this type of heating is sufficient to maintain both the quiet and active corona and that it also has the non-homogeneous temperature distribution observed in the lower corona. The behaviour of some brightening events seen in TRACE data support the proposed convective and shock wave mechanisms. The model offers a possible explanation of a long-standing problem, namely why the corona is so hot.
Key words: plasmas / Sun: corona / Sun: magnetic fields
© ESO, 2006
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.