Conditions for fast magnetic reconnection in astrophysical plasmas

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dc.contributor.author Hanasz, Michał
dc.contributor.author Lesch, Harald
dc.date.accessioned 2012-12-19T09:06:13Z
dc.date.available 2012-12-19T09:06:13Z
dc.date.issued 2003-03-27
dc.identifier.citation Astron.Astrophys. 404 (2003) 389-396
dc.identifier.other doi:10.1051/0004-6361:20030471
dc.identifier.uri http://repozytorium.umk.pl/handle/item/252
dc.description.abstract We investigate favourable circumstances for fast magnetic reconnection in astrophysical plasmas based on recent results by Rogers et al. (2001). Given that a critical magnetic field structure with antiparallel field lines exists, our analysis demonstrates that a sufficient condition for fast reconnection is that the ratio of the thermal pressure to the magnetic field pressure $\beta$ should be significantly larger than $ 2 m_e/m_p$ (twice the ratio of electron mass to proton mass). Using several examples (like the different components of the interstellar medium, the intergalactic medium, active galactic nuclei and jets) we show that in almost all astrophysical plasmas, magnetic reconnection proceeds fast i.e. independent of the resistivity, with a few percent of the Alfv{\'e}n speed. Only for special cases like neutron stars and white dwarfs is $\beta$ smaller than $2 m_e/ m_p$.
dc.language.iso eng
dc.relation.uri http://arxiv.org/abs/astro-ph/0303608
dc.rights info:eu-repo/semantics/openAccess
dc.subject Astrophysics
dc.title Conditions for fast magnetic reconnection in astrophysical plasmas
dc.type info:eu-repo/semantics/article

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