Katharine K. Reeves 1, Terry G. Forbes 2, Jon Linker 3 & Zoran Mikić 3 1 Harvard-Smithsonian Center for Astrophysics 2 University of New Hampshire 3 Science.

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Presentation transcript:

Katharine K. Reeves 1, Terry G. Forbes 2, Jon Linker 3 & Zoran Mikić 3 1 Harvard-Smithsonian Center for Astrophysics 2 University of New Hampshire 3 Science Applications International Corporation Theoretical Predictions of Energy Release in CMEs and Calculations of Flare Emissions Thanks to the NSF-SHINE program for funding this work!

Overview Main Goal: Energy dissipated in the current sheet Flare emissions Methods: 1. Analytic: loss-of- equilibrium model 2. Numerical: 2.5D MHD code (SAIC MAS) Lin & Forbes, 2000

Equilibrium Curve Forbes & Priest, 1995

Poynting Flux Thermalized

Energy Release

Effect of M A on Energy Time (s) Energy (x ergs) M A = M A = M A = 0.1 Reeves & Forbes, ApJ, 2005

Soft X-ray Telescope (SXT) Light Curves Observed Simulated Data from Reeves & Warren, ApJ, 2002 Simulated light curves from Reeves & Forbes, ApJ 2005

Velocities and Light Curves Red curves Blue curves Background Field: 50 G Flux rope mass: 2.1 x gm Background Field: 25 G Flux rope mass: 4.0 x gm

Densities in the flare loops Density Reeves, Warren & Forbes, ApJ, 2007

Simulated Flare Images TRACE 171ÅTRACE 195Å SXT Al12SXT Be119 Reeves, et al., ApJ, 2007

Loop-top knots and bars (e.g. Feldman, et al., 1995) Yohkoh SXTTRACE 171TRACE 195 (e.g. Doschek & Warren, 2005)

SAIC MAS MHD model

Density Temperature

Energy over simulation domain shearing flux cancellation current sheet forms

Current sheet

Energy partition

Energy into current sheet

Energy flow at r0

Energy flow at r1

Simulated light curves

XRT observations

Conclusions The loss-of-equilibrium model is capable of simulating flare emissions characteristic of observations In the SAIC simulations, a higher fraction of the energy leaves the current sheet at the r1 boundary than the r0 boundary.

Conclusions Conduction, viscous flow decrease the energy swept in to the current sheet via the Poynting flux. The bulk of the energy flow at r0 is conductive flux, which can be used as the input to multi-threaded 1D flare loop simulations, as in Reeves et al. (2007).