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Published byGilbert McCoy Modified over 9 years ago
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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, NASALMSALTRACENASA
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RD GDS RD accels plasma GDS heats plasma to flare temp. @ loop top Simulation region 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) MpMp MsMs Chromosphere T=0.01 Corona T=1 Uniform pressure in TR Trans. Reg. (TR) GDS Post-shock Fluid input
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Model loop atmosphere ChromosphereTRCorona
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Time Evolution for the uniform tube
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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 TR Nozzle at the centre of the TR Nozzle above the TR The area profile has a form of a piecewise linear function. ThermalConductionFrontThermalConductionFrontThermalConductionFront
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Transsonic points (lower) (upper)
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Transsonic points (lower) (upper)
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