Explosive heating of low-density coronal plasma

Details Explosive heating of low-density coronal plasma Explosive heating of low-density coronal plasma

Nov 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...458..987b&link_type=abstract

Astronomy and Astrophysics, Volume 458, Issue 3, November II 2006, pp.987-995

Astronomy and Astrophysics

Astrophysics

24

Atomic Processes, Hydrodynamics, Sun: Corona, Sun: Uv Radiation

Scientific paper

Context: .This paper addresses the impulsive heating of very diffuse coronal loops, such as can occur in a nanoflare-heated corona with low filling factor. Aims: .We study the physics associated with nanoflare heating in this scenario and aim to determine whether there exist any observable signatures. Methods: .We derive an analytical model in order to gain some simple physical insights into the system and use a one dimensional hydrodynamic model that treats the electrons and ions as a coupled fluid to simulate nanoflare heating with time-scales of 30 s. Our analytical model also provide a means of verifying our numerical results. Results: .We find that diffuse loops containing plasma at T> 20 MK can be rapidly created and subsequently filled by the violent evaporation of chromospheric plasma driven by near-saturated thermal conduction. Most importantly, we find order-of-magnitude departures from equilibrium of the ionisation balance for iron and use this result to identify a potential signature of this heating mechanism. Conclusions: .We conclude that nanoflare heating can account for the presence of extremely high temperature plasma in a corona with low filling factor. We find that near-saturated thermal conduction may play a key role at the onset of chromospheric evaporation and a non-equilibrium ionisation balance is absolutely inevitable. The high temperatures could never be directly measured in the corona due to the small emission measure and the most promising signature of such heating is blue-shifted plasma from the loop footpoints. We find reason for cautious optimism that this signature can be detected by future space-based spectroscopic instrumentation (e.g. SolarB-EIS).

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