Magnetic topology of actively evolving and passively convecting structures in the turbulent solar wind

Hnat, B., Chapman, S. C. and Watkins, N. W. ORCID: 0000-0003-4484-6588 (2021) Magnetic topology of actively evolving and passively convecting structures in the turbulent solar wind. Physical Review Letters, 126 (12). ISSN 0031-9007

Text (PhysRevLett.126.125101) - Published Version Available under License Creative Commons Attribution. Download (749kB)

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Abstract

Multipoint in situ observations of the solar wind are used to identify the magnetic topology and current density of turbulent structures. We find that at least 35% of all structures are both actively evolving and carrying the strongest currents, actively dissipating, and heating the plasma. These structures are comprised of 1/5 3D plasmoids, 3/5 flux ropes, and 1/5 3D X points consistent with magnetic reconnection. Actively evolving and passively advecting structures are both close to log-normally distributed. This provides direct evidence for the significant role of strong turbulence, evolving via magnetic shearing and reconnection, in mediating dissipation and solar wind heating.

Item Type:	Article
Official URL:	https://journals.aps.org/prl/
Additional Information:	© 2021 American Physical Society
Divisions:	Centre for Analysis of Time Series LSE Health
Subjects:	Q Science > QC Physics Q Science > Q Science (General)
Date Deposited:	30 Apr 2021 13:39
Last Modified:	16 Nov 2024 03:51
URI:	http://eprints.lse.ac.uk/id/eprint/110320

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