Authors: Leon Ofman (CUA/NASA GSFC), Scott A Boardsen (UMBC/NASA GSFC), Lan Jian (NASA GSFC), Yogesh (CUA/NASA GSFC), Jaye Verniero (NASA GSFC), Viacheslav M Sadykov (Georgia State University)

Anisotropic ion beams in the solar wind are observed by the SPAN-I instruments on board the Parker Solar Probe (PSP) spacecraft. The ion beams are often associated with polarized ion-scale waves, and anisotropic velocity distributions that consist of core, beam, and hammerhead (i.e., extended anisotropic strahl) populations. These various parts of the beams exhibit temperature anisotropies, with T⊥/T||>1, and the beam speed is often super-Alfvénic. The alpha particle population VDFs show similar unstable features. Since the wave-particle interactions can play an important role in the energy transfer between the fields and particles leading to solar wind plasma heating, we model the nonlinear evolution of the beams using 2.5D and 3D hybrid models (kinetic ions, and fluid electrons). The models are initialized with bi-Maxwellian core and super-Alfvenic beam distributions with various degrees of anisotropy. We find that the modeled super-Alfvenic anisotropic ion beams are unstable with respect to the magnetosonic and ion-cyclotron instabilities, leading to rapid growth and nonlinear saturation of the instabilities. The emitted kinetic wave spectrum interacts with the beam ion populations, leading to secondary instabilities. The models reproduce the observed kinetic-scale processes detected in-situ by the PSP encounters and demonstrate the transfer of energy between the fields and ions in the solar wind. We use the modeling results for training of Machine Learning algorithms to develop automated identification and classification of ion-kinetic instabilities in the solar wind plasma.