Heating of Minor Ions by the Coronal Slow Shock

The coronal slow shock has been changes of alpha particles' velocity, density, and predicted to exist embedded in large coronal holes temperature have been published, both for fast at 4-10 solar radii. We use a three-fluid model to interplanetary shocks and for the Earth's bow study the jumps in minor ion properties across a slow shock such as the coronal slow shock. We formulate the jump conditions in the de HoffmannTeller frame of reference. The Rankine-Hugoniot solution determines the MHD flow and the magnetic field across the shocks. For each minor ion species, the fluid equations for the conservation of mass, momentum and energy can be solved to determine the velocity and the temperature of the shock [Borodkova et al., 1989; Fuselier et al., 1988; Neugebauer, 1970; Ogilvie et al., 1982; Zastenker et al., 1986]. Both Ogilvie et al. [1982] and Borodkova et al. [1989] reported that reacting to the presence of the cross-shock potential difference the alpha particles are decelerated less than the protons and a temperature-mass proportionality is introduced by the action of a fast shock. It has also been ions across the shock. We also obtain a similarity observed that magnetic forces contribute solution for heavy ions. The results show that on appreciably to the slowing of ions in the de the downstream side of the slow shock the ion Hoffmann-Teller frame of reference [Thomsen et temperatures are nearly proportional to the ion al., 1987]. We expected that slow shocks and fast masses for He, O, Si, and Fe in agreement with shocks may have similar effects on the dynamical observed ion temperatures in the inner solar wind. behavior of solar wind ions. This study concludes This indicates that the possibly existing coronal slow shock can be responsible for the observed heating of minor ions in the solar wind.