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Breakdown of chiral symmetry during saturation of the Tayler instability
Stockholms universitet, Nordiska institutet för teoretisk fysik (Nordita).ORCID-id: 0000-0002-7304-021X
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi. Stockholms universitet, Nordiska institutet för teoretisk fysik (Nordita).
2012 (Engelska)Ingår i: Physical Review E. Statistical, Nonlinear, and Soft Matter Physics, ISSN 1539-3755, E-ISSN 1550-2376, Vol. 86, nr 1, s. 016313-Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

We study spontaneous breakdown of chiral symmetry during the nonlinear evolution of the Tayler instability. We start with an initial steady state of zero helicity. Within linearized perturbation calculations, helical perturbations of this initial state have the same growth rate for either sign of helicity. Direct numerical simulations (DNS) of the fully nonlinear equations, however, show that an infinitesimal excess of one sign of helicity in the initial perturbation gives rise to a saturated helical state. We further show that this symmetry breaking can be described by weakly nonlinear finite-amplitude equations with undetermined coefficients which can be deduced solely from symmetry consideration. By fitting solutions of the amplitude equations to data from DNS, we further determine the coefficients of the amplitude equations.

Ort, förlag, år, upplaga, sidor
2012. Vol. 86, nr 1, s. 016313-
Nationell ämneskategori
Matematisk analys
Identifikatorer
URN: urn:nbn:se:su:diva-80437DOI: 10.1103/PhysRevE.86.016313ISI: 000306415900005OAI: oai:DiVA.org:su-80437DiVA, id: diva2:555364
Anmärkning

AuthorCount:4;

Tillgänglig från: 2012-09-19 Skapad: 2012-09-19 Senast uppdaterad: 2024-02-07Bibliografiskt granskad
Ingår i avhandling
1. From irrotational flows to turbulent dynamos
Öppna denna publikation i ny flik eller fönster >>From irrotational flows to turbulent dynamos
2012 (Engelska)Doktorsavhandling, sammanläggning (Övrigt vetenskapligt)
Abstract [en]

Many of the celestial bodies we know are found to be magnetized:the Earth, many of the planets so far discovered, the Sun and other stars,the interstellar space, the Milky Way and other galaxies.The reason for that is still to be fully understood, and this work is meant to be a step in that direction.

The dynamics of the interstellar medium is dominated by events likesupernovae explosions that can be modelled as irrotational flows.The first part of this thesis is dedicated to the analysis of some characteristics of these flows, in particular how they influencethe typical turbulent magnetic diffusivity of a medium, and it is shownthat the diffusivity is generally enhanced, except for some specific casessuch as steady potential flows, where it can be lowered.Moreover, it is examined how such flows can develop vorticity when they occur in environments affected by rotation or shear,or that are not barotropic.

Secondly, we examine helical flows, that are of basic importance for the phenomenon of the amplification of magnetic fields, namely the dynamo.Magnetic helicity can arise from the occurrence of an instability: here we focus on theinstability of purely toroidal magnetic fields, also known as Tayler instability.It is possible to give a topological interpretation of magnetic helicity.Using this point of view, and being aware that magnetic helicity is a conserved quantity in non-resistive flows,it is illustrated how helical systems preserve magnetic structureslonger than non-helical ones.

The final part of the thesis deals directly with dynamos.It is shown how to evaluate dynamo transport coefficients with two of the most commonly used techniques, namely theimposed-field and the test-field methods.After that, it is analyzed how dynamos are affected by advectionof magnetic fields and material away from the domain in which theyoperate.It is demonstrated that the presence of an outflow, likestellar or galactic winds in real astrophysical cases,alleviates the so-calledcatastrophic quenching, that is the damping of a dynamoin highly conductive media, thus allowing the dynamo process to work better.

Ort, förlag, år, upplaga, sidor
Stockholm: Department of Astronomy, Stockholm University, 2012. s. 76
Nyckelord
astrophysics, magnetic fields, insterstellar medium, MHD, dynamo, turbulence, instability
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Forskningsämne
astronomi
Identifikatorer
urn:nbn:se:su:diva-80958 (URN)978-91-7447-573-9 (ISBN)
Disputation
2012-11-14, sal FB52, AlbaNova universitetscentrum, Roslagstullsbacken 21, Stockholm, 10:15 (Engelska)
Opponent
Handledare
Anmärkning

At the time of the doctoral defence the following paper was unpublished and had a status as follows: Paper nr 5: Submitted

Tillgänglig från: 2012-10-23 Skapad: 2012-10-03 Senast uppdaterad: 2022-02-24Bibliografiskt granskad

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Brandenburg, AxelDel Sordo, Fabio

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Brandenburg, AxelDel Sordo, Fabio
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Nordiska institutet för teoretisk fysik (Nordita)Institutionen för astronomi
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Physical Review E. Statistical, Nonlinear, and Soft Matter Physics
Matematisk analys

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