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Slow magnetosonic waves associated with flares were observed in coronal loopsby SOHO/SUMER, SDO/AIA in various EUV bandpasses, and other instruments. Theexcitation and damping of slow magnetosonic waves provides information on themagnetic, temperature, and density structure of the loops. Recently, it wasfound using 1.5D models that the thermal conduction is suppressed andcompressive viscosity is enhanced in hot (T>6 MK) flaring coronal loops. Wemodel the excitation and dissipation of slow magnetosonic waves in hot coronalloops with realistic magnetic geometry, enhanced density, and temperature(compared to background corona) guided by EUV observations using 3D MHDvisco-resistive model. The effects of compressive viscosity tensor componentalong the magnetic field are included with classical and enhanced viscositycoefficient values for the first time in 3D MHD coronal loop model. The wavesare excited by a velocity pulse at the footpoint of the loop at coronal lowerboundary. The modeling results demonstrate the excitation of the slowmagnetosonic waves and nonlinear coupling to other wave modes, such as the kinkand fast magnetosonic. We find significant leakage of the waves from the hotcoronal loops with small effect of viscous dissipation in cooler (6MK) loops,and more significant effects of viscous dissipation in hotter (10.5MK) coronalloops. Our results demonstrate that nonlinear 3D MHD models are required tofully account for various wave couplings, damping, standing wave formation, andviscous dissipation in hot flaring coronal loops. Our viscous 3D MHD codeprovides a new tool for improved coronal seismology.

Excitation and Damping of Slow Magnetosonic Waves in Flaring Hot Coronal Loops: Effects of Compressive Viscosity