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

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 escap...

Full description

Saved in:
Bibliographic Details
Main Authors: 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
Format: Article
Language:English
Published: IOP Publishing 2025-01-01
Series:The Astrophysical Journal
Subjects:
Solar wind
Slow solar wind
Alfvén waves
Chemical abundances
Online Access:https://doi.org/10.3847/1538-4357/ada699
Tags: Add Tag
No Tags, Be the first to tag this record!

Internet

https://doi.org/10.3847/1538-4357/ada699

Similar Items