An evaluation of possible mechanisms for anomalous resistivity in the solar corona

dc.contributor.author	Singh, K.A.P.
dc.contributor.author	Subramanian, P.
dc.date.accessioned	2021-09-22T10:03:01Z
dc.date.available	2021-09-22T10:03:01Z
dc.date.issued	2007-07
dc.identifier.issn	1573093X
dc.identifier.uri	http://localhost:8080/xmlui/handle/123456789/1710
dc.description.abstract	A wide variety of transient events in the solar corona seem to require explanations that invoke fast reconnection. Theoretical models explaining fast reconnection often rely on enhanced resistivity. We start with data derived from observed reconnection rates in solar flares and seek to reconcile them with the chaos-induced resistivity model of Numata and Yoshida (Phys. Rev. Lett. 88, 045003, 2002) and with resistivity arising out of the kinetic Alfvén wave (KAW) instability. We find that the resistivities arising from either of these mechanisms, when localized over length scales of the order of an ion skin depth, are capable of explaining the observationally mandated Lundquist numbers.	en_US
dc.description.sponsorship	Solar Physics	en_US
dc.language.iso	en	en_US
dc.relation.ispartofseries	Issue 2;Volume 243
dc.subject	solar corona;	en_US
dc.subject	enhanced resistivity;	en_US
dc.subject	ion skin depth;	en_US
dc.title	An evaluation of possible mechanisms for anomalous resistivity in the solar corona	en_US
dc.type	Article	en_US