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E and B Polarizations from Inhomogeneous and Solar Surface Turbulence
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.ORCID iD: 0000-0002-7304-021X
Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.;Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.;Ilia State Univ, Abastumani Astrophys Observ, 3-5 Cholokashvili St, GE-0194 Tbilisi, Rep of Georgia..
Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.;Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA..
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2019 (English)In: Astrophysical Journal, ISSN 0004-637X, Vol. 870, no 2, article id 87Article in journal (Refereed) Published
Abstract [en]

Gradient- and curl-type or E- and B-type polarizations have been routinely analyzed to study the physics contributing to the cosmic microwave background polarization and galactic foregrounds. They characterize the parity-even and parity-odd properties of the underlying physical mechanisms, such as, for example, hydromagnetic turbulence in the case of dust polarization. Here, we study spectral correlation functions characterizing the parity-even and parity-odd parts of linear polarization for homogeneous and inhomogeneous turbulence to show that only the inhomogeneous helical case can give rise to a parity-odd polarization signal. We also study nonhelical turbulence and suggest that a strong non-vanishing (here negative) skewness of the E polarization is responsible for an enhanced ratio of the EE to the BB (quadratic) correlation in both the helical and nonhelical cases. This could explain the enhanced EE/BB ratio observed recently for dust polarization. We close with a preliminary assessment of using the linear polarization of the Sun to characterize its helical turbulence without being subjected to the pi ambiguity that magnetic inversion techniques have to address.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2019. Vol. 870, no 2, article id 87
Keywords [en]
dynamo, magnetohydrodynamics (MHD), Sun: magnetic fields, turbulence
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-242979DOI: 10.3847/1538-4357/aaf383ISI: 000455820100033Scopus ID: 2-s2.0-85060253289OAI: oai:DiVA.org:kth-242979DiVA, id: diva2:1286320
Note

QC 20190206

Available from: 2019-02-06 Created: 2019-02-06 Last updated: 2019-02-06Bibliographically approved

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Brandenburg, Axel

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