Coronal heating by magnetic kink waves

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DC Field	Value	Language
dc.contributor.author	Banerjee, D	-
dc.contributor.author	Dikpati, M	-
dc.contributor.author	Choudhuri, A. R	-
dc.date.accessioned	2009-06-03T10:58:17Z	-
dc.date.available	2009-06-03T10:58:17Z	-
dc.date.issued	1998	-
dc.identifier.citation	Chan, K.L., Cheng, K.S and Singh, H.P eds., 1997 Pacific Rim conference on Stellar Astrophysics., Proceedings of ASP Conference Hongkong, PRC, 13 - 16 August, 1997., pp. 15 - 18	en
dc.identifier.isbn	1-886733-58-9	-
dc.identifier.uri	http://hdl.handle.net/2248/4506	-
dc.description.abstract	We show that the magnetic kink waves generated by the motions of the Photospheric footpoints of the coronal flux tubes can supply adequate energy for heating the quiet corona. We model the solar corona as two-layer isothermal atmosphere, with the lower layer having chromospheric thickness and the temperature and the upper layer having coronal temperature	en
dc.language.iso	en	en
dc.publisher	Astronomical Society of the Pacific	en
dc.relation.ispartofseries	Astronomical Society of a Pacific Conference Series; Vol. 138	-
dc.relation.uri	http://adsabs.harvard.edu/abs/1998ASPC..138...15B	en
dc.rights	© Astronomical Society of the Pacific	en
dc.subject	Coronal heating	en
dc.subject	Magnetic kink waves	en
dc.subject	Stellar astrophysics	en
dc.title	Coronal heating by magnetic kink waves	en
dc.type	Article	en
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