Differentiating the Acceleration Mechanisms in the Slow and Alfvénic Slow Solar Wind

In the corona, plasma is accelerated to hundreds of kilometers per second and heated to temperatures hundreds of times hotter than the Sun's surface before it escapes to form the solar wind. Decades of space-based experiments have shown that the energization process does not stop after it escapes. I...

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Autori principali:	Yeimy J. Rivera, Samuel T. Badman, J. L. Verniero, Tania Varesano, Michael L. Stevens, Julia E. Stawarz, Katharine K. Reeves, Jim M. Raines, John C. Raymond, Christopher J. Owen, Stefano A. Livi, Susan T. Lepri, Enrico Landi, Jasper. S. Halekas, Tamar Ervin, Ryan M. Dewey, Rossana De Marco, Raffaella D’Amicis, Jean-Baptiste Dakeyo, Stuart D. Bale, B. L. Alterman
Natura:	Artigo
Lingua:	Inglês
Pubblicazione:	IOP Publishing 2025-01-01
Serie:	The Astrophysical Journal
Soggetti:	Solar wind Slow solar wind Alfvén waves Chemical abundances
Accesso online:	https://doi.org/10.3847/1538-4357/ada699
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