Coronal magnetic loops

V.V. Zaitsev^a, A.V. Stepanov^b
^aFederal Research Center A.V. Gaponov-Grekhov Institute of Applied Physics of the Russian Academy of Sciences, ul. Ulyanova 46, Nizhny Novgorod, 603000, Russian Federation
^bThe Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, Pulkovskoe shosse 65/1, St. Petersburg, 196140, Russian Federation

The goal of this review is to outline some new ideas in the physics of coronal magnetic loops, the fundamental structural elements of the atmospheres of the Sun and flaring stars, which are involved in phenomena such as stellar coronal heating, flare energy release, charged particle acceleration, and the modulation of optical, radio, and X-ray emissions. The Alfvén — Carlqvist view of a coronal loop as an equivalent electric circuit allows a good physical understanding of loop processes. Describing coronal loops as MHD-resonators explains various ways in which flaring emissions from the Sun and stars are modulated, whereas modeling them by magnetic mirror traps allows one to describe the dynamics and emission of high-energy particles. Based on these approaches, loop plasma and fast particle parameters are obtained and models for flare energy release and stellar corona heating are developed.

PACS: 52.35.−g, 96.60.−j, 97.10.Sj (all)
DOI: 10.1070/PU2008v051n11ABEH006657
URL: https://ufn.ru/en/articles/2008/11/b/
Web of Science

000264020300002
Scopus

2-s2.0-68149161150
ADS NASA

2008PhyU...51.1123Z
Citation: Zaitsev V V, Stepanov A V "Coronal magnetic loops" Phys. Usp. 51 1123–1160 (2008)

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Оригинал: Зайцев В В, Степанов А В «Корональные магнитные арки» УФН 178 1165–1204 (2008); DOI: 10.3367/UFNr.0178.200811b.1165

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