Diffusion of large-scale magnetic fields by reconnection in MHD turbulence

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dc.creatorReinaldo Santos de Lima
dc.creatorGustavo Andres Guerrero Eraso
dc.creatorElisabete Maria de Gouveia Dal Pino
dc.creatorAlex Lazarian
dc.date.accessioned2023-11-13T16:34:45Z
dc.date.accessioned2025-09-09T01:03:12Z
dc.date.available2023-11-13T16:34:45Z
dc.date.issued2021
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulo
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1093/mnras/stab470
dc.identifier.issn1365-2966
dc.identifier.urihttps://hdl.handle.net/1843/60871
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Aberto
dc.subjectCampos magnéticos
dc.subjectEstrelas
dc.subjectDifusão
dc.subject.otherMagnetic fields
dc.subject.otherMagnetic reconnection
dc.subject.otherMagnetohydrodynamic
dc.subject.otherTurbulence
dc.subject.otherStars
dc.titleDiffusion of large-scale magnetic fields by reconnection in MHD turbulence
dc.typeArtigo de periódico
local.citation.epage1309
local.citation.issue1
local.citation.spage1290
local.citation.volume503
local.description.resumoThe rate of magnetic field diffusion plays an essential role in several astrophysical plasma processes. It has been demonstrated that the omnipresent turbulence in astrophysical media induces fast magnetic reconnection, which consequently leads to large-scale magnetic flux diffusion at a rate independent of the plasma microphysics. This process is called 'reconnection diffusion' (RD) and allows for the diffusion of fields, which are dynamically important. The current theory describing RD is based on incompressible magnetohydrodynamic (MHD) turbulence. In this work, we have tested quantitatively the predictions of the RD theory when magnetic forces are dominant in the turbulence dynamics (Alfvénic Mach number MA < 1). We employed the Pencil Code to perform numerical simulations of forced MHD turbulence, extracting the values of the diffusion coefficient ηRD using the test-field method. Our results are consistent with the RD theory (⁠ηRD∼M3A for MA < 1) when turbulence approaches the incompressible limit (sonic Mach number MS ≲ 0.02), while for larger MS the diffusion is faster (⁠ηRD∼M2A⁠). This work shows for the first time simulations of compressible MHD turbulence with the suppression of the cascade in the direction parallel to the mean magnetic field, which is consistent with incompressible weak turbulence theory. We also verified that in our simulations the energy cascading time does not follow the scaling with MA predicted for the weak regime, in contradiction with the RD theory assumption. Our results generally support and expand the RD theory predictions.
local.identifier.orcidhttps://orcid.org/0000-0001-6880-4468
local.identifier.orcidhttps://orcid.org/0000-0002-2671-8796
local.identifier.orcidhttps://orcid.org/0000-0001-8058-4752
local.identifier.orcidhttps://orcid.org/0000-0002-7336-6674
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnras/article/503/1/1290/6144594

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