On solar coronal heating

dc.contributor.author	Pandey, K
dc.contributor.author	Narain, U
dc.date.accessioned	2008-04-22T07:11:04Z
dc.date.available	2008-04-22T07:11:04Z
dc.date.issued	2001
dc.identifier.citation	BASI, Vol. 29, No. 3, pp. 231 - 238	en
dc.identifier.uri	http://hdl.handle.net/2248/2244
dc.description.abstract	We review heating of solar corona by magnetic fields/currents. Our emphasis is on micro- and nano-flares. In case of a microflare the energy release is ~1026 ergs whereas in a nanoflare ~1023 - 1025 ergs of energy is released. Flares have a distribution law over total radiated energy with exponent α = 1.8. Extending the same power law to micro-and nano-flares and assuming that they constitute a dominant heating mechanism for solar corona ??must be greater than 2. Many investigations lead to α < 2 whereas a few yield α > 2. The verdict remains inconclusive. More observational analyses and numerical simulations are needed to discriminate between the two cases.	en
dc.format.extent	653694 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Astronomical Society of India	en
dc.relation.uri	http://adsabs.harvard.edu/abs/2001BASI...29..231P	en
dc.subject	Coronal heating	en
dc.subject	Solar corona	en
dc.title	On solar coronal heating	en
dc.type	Article	en