Shock formation of slow magnetosonic waves in coronal plumes

We investigate the height of shock formation in coronal plumes for slow magnetosonic waves. The models take into account plume geometric spreading, heat conduction, and radiative damping. The wave parameters as well as the spreading functions of the plumes and the base magnetic field strength are given by empirical constraints mostly from the Solar and Heliospheric Observatory/Ultraviolet Coronagraph Spectrometer. Our models show that shock formation occurs at low coronal heights, i.e., within 1.3 R-., depending on the wave parameters. The R, shock formation is calculated using the well-established wave-breaking condition given by the intersection of C+ characteristics in the space-time plane. Our models show that shock heating by slow magnetosonic waves is expected to be relevant at most heights in solar coronal plumes, although slow magnetosonic waves are most likely not a solely operating energy supply mechanism.