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The effects of canopy expansion on chromospheric evaporation driven by thermal
conduction fronts
Authors: F. Rozpedek, S. R. Brannon, D. W. Longcope
Credit: M. Aschwanden et al. (LMSAL), TRACE, NASA
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RD RDGDSGDS
RD accels plasma
GDS heats plasma to flare temp. @
loop top
Simulationregion
Chromosphere
Reconnection frees loop to
contract
~90% free mag. energy => bulk plasma motion(Longcope et al. 2009)
Flare loop dynamics
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1-D “shocktube” model
•Model details:
•Static non-uniform grid:
• <1 km (chromosphere), ~10 km (corona), scales up in TR
•Include viscosity & Spitzer conductivity
•Neglect gravity & explicit radiative effects
•Simplified model atmosphere: temp. grad. @ const.
pressure
•Classical piston shock (tanh func. w/ Rankine-
Hugoniot)
Mp
Ms
ChromosphereT=0.01
CoronaT=1
Uniform pressure in TR
Trans. Reg.(TR)
GDS
Post-shockFluidinput
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Model loop atmosphereChromosphere TR Corona
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Time Evolution for the uniform tube
TCF
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Time Evolution for the uniform tube
TCF
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Time Evolution for the uniform tube
E
C
TCF
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Time Evolution for the uniform tube
E
C
TCFC
E
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Time Evolution for the uniform tubeE
C
TCF
CE
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A
CB
TR ??
Question:Is there some observational quantity that would enable us to determine where the nozzle is located relative to the Transition Region?
The canopy expansion
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Varying Area Profile
Nozzle below the TRNozzle at the centre
of the TR Nozzle above the TR
The area profile has a form of a piecewise linear function.
ThermalConduction
Front
ThermalConduction
Front
ThermalConduction
Front
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Transsonic points(lower) (upper)
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Transsonic points (lower) (upper)
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Thank You