Modeling radio scattering and scintillation observations of the inner solar wind using oblique Alfvén/ion cyclotron waves

Radio scattering and scintillation observations of the near‐Sun solar wind are shown to be dominated by effects associated with obliquely propagating Alfvén/ion cyclotron waves. We base this on a modeling of structure functions from angular/spectral broadening observations and velocity measurements from interplanetary scintillation (IPS) observations. A simple damped‐WKB model was found inadequate, as Landau damping erodes the spectrum faster than is consistent with the observed inner scale. Invoking a turbulent cascade can counteract this damping and push the spectral cutoff back out to the observed inner scale near the ion inertial scale. Adjusting the spectrum amplitude and cascade rate to match observations gives an estimate of the wave dissipation power associated with electron Landau damping and proton cyclotron damping. The implied power levels are substantial, being comparable with levels typically invoked in extended wave heating models. Both the shape and the amplitude of the observed structure functions can be explained by a composite spectrum made up of a power law component of passive or non‐Alfvénic density fluctuations and a local flattening associated with the enhanced linear Alfvén wave compressibility at small (ion cyclotron) scales. Since IPS is dominated by the enhanced small‐scale density fluctuations, the scintillation velocity field should show a strong wave effect. Our modeling of IPS velocities does, in fact, show that the large parallel velocity spread and upward bias to the mean velocity observed near the Sun are a direct result of the density fluctuations associated with Alfvén waves along an extended line of sight.