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