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Observed Low-Plasma- βTemperature Anisotropy Constraint Driven byα -Particle Drift
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Observed Low-Plasma- βTemperature Anisotropy Constraint Driven byα -Particle Drift

Mihailo M Martinović, Kristopher G Klein, Leon Ofman, Yogesh, Jaye L Verniero, Peter H Yoon, Gregory G Howes, Daniel Verscharen and Benjamin L Alterman
ArXiv.org
Cornell University
12/20/2025
DOI: 10.48550/arxiv.2512.18485
url
https://doi.org/10.48550/arxiv.2512.18485View
Preprint (Author's original)This preprint has not been evaluated by subject experts through peer review. Preprints may undergo extensive changes and/or become peer-reviewed journal articles. Open Access

Abstract

Some plasma instability thresholds, derived from linear theory, constrain the observed parameters of solar wind velocity distributions, defining boundaries of ``allowed'' plasma parameters. These thresholds typically account for a single source of free energy, such as temperature anisotropy or a drifting secondary component with some dependence on other system parameters, e.g. the ratio of thermal to magnetic pressure,$β$ . Excursions beyond these thresholds result in the emission of energy, transferred from particles to coherent electromagnetic waves, acting to push the system toward a more stable configuration. In this work, we use linear theory to define parametric limits for a low- $β$plasma that contains a drifting proton beam or helium ( $α$ )-particle population. A sufficiently fast and dense drifting population triggers an Oblique Drift Instability (ODI). This instability decreases the velocity drift between the thermal proton and secondary populations and prevents$β$from decreasing below a minimum value by heating both the core and drifting populations. Our predictions are of interest for Parker Solar Probe observations, as they provide an additional mechanism for perpendicular heating of ions active in the vicinity of surface. The ODI also explains the discrepancy between long-standing expectations of measurements of very low- $β$plasmas with very large temperature anisotropies in the near-Sun environment and in situ observations, where$β$is consistently measured above a few percent and the secondary populations drifting faster than the bulk of proton population by no more than approximately one velocity.
 Physics - Solar and Stellar Astrophysics

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