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Compensating Faraday Depolarization by Magnetic Helicity in the Solar Corona
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA; Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80303, USA; Department of Astronomy, AlbaNova University Center, Stockholm University, SE-10691 Stockholm, Sweden.ORCID iD: 0000-0002-7304-021X
2017 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 845, no 2, article id L15Article in journal (Refereed) Published
Abstract [en]

A turbulent dynamo in spherical geometry with an outer corona is simulated to study the sign of magnetic helicity in the outer parts. In agreement with earlier studies, the sign in the outer corona is found to be opposite to that inside the dynamo. Line-of-sight observations of polarized emission are synthesized to explore the feasibility of using the local reduction of Faraday depolarization to infer the sign of helicity of magnetic fields in the solar corona. This approach was previously identified as an observational diagnostic in the context of galactic magnetic fields. Based on our simulations, we show that this method can be successful in the solar context if sufficient statistics are gathered by using averages over ring segments in the corona separately for the regions north and south of the solar equator.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD , 2017. Vol. 845, no 2, article id L15
Keywords [en]
dynamo, magnetohydrodynamics (MHD), Sun: magnetic fields, turbulence
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-214332DOI: 10.3847/2041-8213/aa844bISI: 000407971200003Scopus ID: 2-s2.0-85028457905OAI: oai:DiVA.org:kth-214332DiVA, id: diva2:1140520
Note

QC 20170912

Available from: 2017-09-12 Created: 2017-09-12 Last updated: 2017-09-12Bibliographically approved

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Brandenburg, Axel

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