Kinetic-scale Current Sheets in Near-Sun Solar Wind: Properties, Scale-dependent Features and Reconnection Onset

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Lotekar, AjayUppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen (author)

Kinetic-scale Current Sheets in Near-Sun Solar Wind : Properties, Scale-dependent Features and Reconnection Onset

Article/chapterEnglish2022

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2022-04-12
American Astronomical Society,2022
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LIBRIS-ID:oai:DiVA.org:uu-473550
https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-473550URI
https://doi.org/10.3847/1538-4357/ac5bd9DOI

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Language:English
Summary in:English

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We present statistical analysis of 11,200 proton kinetic-scale current sheets (CS) observed by the Parker Solar Probe during 10 days around the first perihelion. The CS thickness lambda is in the range from a few to 200 km with the typical value around 30 km, while current densities are in the range from 0.1 to 10 mu A m(-2) with the typical value around 0.7 mu A m(-2). These CSs are resolved thanks to magnetic field measurements at 73-290 samples s(-1) resolution. In terms of proton inertial length lambda(p), the CS thickness lambda is in the range from about 0.1 to 10 lambda(p) with the typical value around 2 lambda(p). The magnetic field magnitude does not substantially vary across the CSs, and accordingly the current density is dominated by the magnetic-field-aligned component. The CSs are typically asymmetric with statistically different magnetic field magnitudes at the CS boundaries. The current density is larger for smaller-scale CSs, J(0) approximate to 0.15 x (lambda/100 km)(-0.76) mu A m(-2), but does not statistically exceed the Alfven current density J(A) corresponding to the ion-electron drift of the local Alfven speed. The CSs exhibit remarkable scale-dependent current density and magnetic shear angles, J(0)/J(A) approximate to 0.17 x (lambda/lambda(p))(-0.67) and Delta theta approximate to 21 degrees x (lambda/lambda(p))(0.32). Based on these observations and comparison to recent studies at 1 au, we conclude that proton kinetic-scale CSs in the near-Sun solar wind are produced by turbulence cascade, and they are automatically in the parameter range, where reconnection is not suppressed by the diamagnetic mechanism, due to their geometry dictated by turbulence cascade.

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Vasko, I. Y.Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.;Russian Acad Sci, Space Res Inst, Moscow, Russia. (author)
Phan, T.Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. (author)
Bale, S. D.Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.;Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. (author)
Bowen, T. A.Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. (author)
Halekas, J.Univ Iowa, Iowa City, IA 52242 USA. (author)
Artemyev, A. , V (author)
Khotyaintsev, Yuri V.Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen(Swepub:uu)ykh28990 (author)
Mozer, F. S.Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.;Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. (author)
Uppsala universitetInstitutet för rymdfysik, Uppsalaavdelningen (creator_code:org_t)

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In:Astrophysical Journal: American Astronomical Society929:10004-637X1538-4357

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By the author/editor: Lotekar, Ajay; Vasko, I. Y.; Phan, T.; Bale, S. D.; Bowen, T. A.; Halekas, J.; show more...; Artemyev, A. , V; Khotyaintsev, Yu ...; Mozer, F. S.; show less...

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