Observing the formation of flare-driven coronal rain

@article{Scullion2016ObservingTF,
  title={Observing the formation of flare-driven coronal rain},
  author={Eamon Scullion and Luc H. M. Rouppe van der Voort and Patrick Antolin and Sven Wedemeyer and Gregal J. M. Vissers and Eduard P. Kontar and Peter T. Gallagher},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2016}
}
Flare-driven coronal rain can manifest from rapidly cooled plasma condensations near coronal loop-tops in thermally unstable post-flare arcades. We detect 5 phases that characterise the post-flare decay: heating, evaporation, conductive cooling dominance for ~120 s, radiative / enthalpy cooling dominance for ~4700 s and finally catastrophic cooling occurring within 35-124 s leading to rain strands with s periodicity of 55-70 s. We find an excellent agreement between the observations and model… 
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References

SHOWING 1-10 OF 86 REFERENCES
The multi-thermal and multi-stranded nature of coronal rain
In this work, we analyse coordinated observations spanning chromospheric, TR and coronal temperatures at very high resolution which reveal essential characteristics of thermally unstable plasmas.
Catastrophic cooling and high-speed downflow in quiescent solar coronal loops observed with TRACE
AbstractObservations with the Transition Region and Coronal Explorer, TRACE, show frequent catastrophic cooling and evacuation of quiescent solar coronal loops over active regions. We analyze this
A Numerical Simulation of Cooling Coronal Flare Plasma
We have simulated the cooling of coronal flare plasma (T/sub e/>10/sup 7/ K) using a numerical model of a vertical magnetic flux tube containing an idealized flare chromosphere, transition region,
Dynamics of solar coronal loops II. Catastrophic cooling and high-speed downflows
This work addresses the problem of plasma condensation and "catastrophic cooling" in solar coronal loops. We have carried out numerical calculations of coronal loops and find several classes of
CATASTROPHIC COOLING OF IMPULSIVELY HEATED CORONAL LOOPS
The physical mechanisms that cause the heating of the solar corona are still far from being completely understood. However, recent highly resolved observations with the current solar missions have
SIGNATURES OF IMPULSIVE LOCALIZED HEATING IN THE TEMPERATURE DISTRIBUTION OF MULTI-STRANDED CORONAL LOOPS
We study the signatures of coronal heating on the differential emission measure (DEM) by means of hydrodynamic simulations capable of resolving the chromospheric-corona transition region sections of
CORONAL RAIN AS A MARKER FOR CORONAL HEATING MECHANISMS
Reported observations in Hα ,C aii H, and K or other chromospheric lines of coronal rain trace back to the days of the Skylab mission. Corresponding to cool and dense plasma, coronal rain is often
THE COOLING OF CORONAL PLASMAS. IV. CATASTROPHIC COOLING OF LOOPS
We examine the radiative cooling of coronal loops and demonstrate that the recently identified catastrophic cooling is due to the inability of a loop to sustain radiative/enthalpy cooling below a
Cooling of solar flares plasmas. 1: Theoretical considerations
Theoretical models of the cooling of flare plasma are reexamined. By assuming that the cooling occurs in two separate phase where conduction and radiation, respectively, dominate, a simple analytic
PLASMA SLOSHING IN PULSE-HEATED SOLAR AND STELLAR CORONAL LOOPS
There is evidence that coronal heating is highly intermittent, and flares are the high energy extreme. The properties of the heat pulses are difficult to constrain. Here hydrodynamic loop modeling
...
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4
5
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