On the Fractal Structure of Solar Supergranulation

dc.contributor.author	Paniveni, U.
dc.contributor.author	Krishan, Vinod
dc.contributor.author	Singh, J.S.
dc.contributor.author	Srikanth, R.
dc.date.accessioned	2007-04-09T11:07:47Z
dc.date.available	2007-04-09T11:07:47Z
dc.date.issued	2005-09
dc.description	Restricted Access.	en
dc.description.abstract	We employ fractal analysis to study the complexity of supergranulation structure using the Solar and Heliospheric Observatory (SOHO) dopplergrams. Our data consists of 200 visually selected supergranular cells, for which we find a broad, slightly asymmetric dispersion in the size distribution, with the most probable size around 31.9 Mm. From the area–perimeter relation, we deduce a fractal dimension D of about 1.25. This is consistent with that for isobars, and suggests a possible turbulent origin of supergranulation. By relating this to the variances of kinetic energy, temperature and pressure, it is concluded that the supergranular network is close to being isobaric and that it has a possible turbulent origin.	en
dc.format.extent	605300 bytes
dc.format.mimetype	application/pdf
dc.identifier.citation	Solar Physics, 2005, Vol.231, p1-10	en
dc.identifier.issn	0038-0938
dc.identifier.uri	http://hdl.handle.net/2289/2253
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.uri	http://dx.doi.org/10.1007/s11207-005-1591-7	en
dc.rights	2005 Springer	en
dc.title	On the Fractal Structure of Solar Supergranulation	en
dc.type	Article	en

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