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In situ observations of large amplitude Alfvén waves heating and accelerating the solar wind
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In situ observations of large amplitude Alfvén waves heating and accelerating the solar wind

Yeimy J Rivera, Samuel T Badman, Michael L Stevens, Jaye L Verniero, Julia E Stawarz, Chen Shi, Jim M Raines, Kristoff W Paulson, Christopher J Owen, Tatiana Niembro, …
ArXiv.org
Cornell University
08/30/2024
DOI: 10.48550/arxiv.2409.00267
url
https://doi.org/10.1126/science.adk6953View
Published (Version of record)This article has now been published in a journal and has been peer-reviewed by subject experts. This version may differ significantly from the preprint version. Access restricted to faculty, staff and students
url
https://doi.org/10.48550/arxiv.2409.00267View
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

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Abstract

After leaving the Sun's corona, the solar wind continues to accelerate and cools, but more slowly than expected for a freely expanding adiabatic gas. We use in situ measurements from the Parker Solar Probe and Solar Orbiter spacecrafts to investigate a stream of solar wind as it traverses the inner heliosphere. The observations show heating and acceleration of the the plasma between the outer edge of the corona and near the orbit of Venus, in connection to the presence of large amplitude Alfvén waves. Alfvén waves are perturbations in the interplanetary magnetic field that transport energy. Our calculations show the damping and mechanical work performed by the Alfvén waves is sufficient to power the heating and acceleration of the fast solar wind in the inner heliosphere.
Physics - Plasma Physics Physics - Solar and Stellar Astrophysics Physics - Space Physics

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