- Conference date: 17–22 June 2012
- Location: Big Island, Hawaii
The fast solar wind results from strong ion heating perpendicular to the coronal hole magnetic field. Kinetic modeling of this ion heating in the expanding collisionless coronal hole must also take into account the effects of gravity, charge-separation electric field, mirror force, inertial force in the accelerating plasma, and ponderomotive Alfvén wave pressure. In Isenberg & Vasquez (ApJ, 731, 88, 2011), we used resonant dissipation of oblique ion-cyclotron waves to yield a reasonable solar wind flow. In that work, the wave intensities were "balanced", with equal power in outward-propagating and sunward-propagating waves. Here, we consider the imbalanced case where the outward-propagating intensities are larger than the sunward intensities, as would be expected from reflection models of turbulent evolution in the solar atmosphere. We present model proton distributions for the case of I + = 4 I − for r = 2 - 4 Rs and compare these proton properties with our earlier balanced model.
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