# Conditions for fast magnetic reconnection in astrophysical plasmas

## Repository of Nicolaus Copernicus University

 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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