Episodic Coronal Loop Heating

Details Episodic Coronal Loop Heating Episodic Coronal Loop Heating

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..261m&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Physics

Coronal Heating, Coronal Loops, Transition Region, Hydrodynamics.

Scientific paper

Coronal loop temperatures are known to be of a few millions degrees but the nature of the energy source remains as a longstanding fundamental problem for solar (and stellar) physics. Observations of solar atmospheric plasma show clear evidence of frequent very localised heating events, which may be statistically responsible for heating of the solar upper atmosphere. One heating theory indicates that these micro-scale events are driven by localized magnetic field reconnection. In this paper, we present the results of numerical calculations that describe the response of the coronal plasma to small-scale heating pulses in a magnetic loop. In particular, we study the effects of energy input pulses injected randomly near the two footpoints of a semi-circular loop. We have found that increasing the elapsing time between successive pulses, the overall loop temperature decreases. When a critical elapsing time is reached the loop can no longer be maintained at typical coronal temperatures. These features have some support from SOHO-CDS observations of coronal loops which seem to undergo strong variability especially in active regions of the solar atmosphere (Kjeldseth-Moe &Brekke, 1998). We also have found that successive random pulses can statistically maintain the average plasma temperature at typical coronal values. Due to the randomness of the heat injections, the resulting temperature profiles show thermal bumps that could be connected to intermittent behaviour in the transition region and the low corona.

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