A phenomenological, kinematical model of the coronal magnetic fields in terms of thin flux tubes rising from the photosphere

dc.contributor.author	Gokhale, M. H
dc.contributor.author	Venkatakrishnan, P
dc.date.accessioned	2009-06-22T15:10:26Z
dc.date.available	2009-06-22T15:10:26Z
dc.date.issued	1978-11
dc.identifier.citation	Pramana, Vol. 11, No. 5, pp. 547 - 558	en
dc.identifier.issn	0304-4289
dc.identifier.uri	http://hdl.handle.net/2248/4569
dc.description.abstract	A kinematical model is necessary for understanding the gross structure of the coronal magnetic field and its slow evolution in consistency with the small scale structure of the photospheric fields. Here we have developed a preliminary phenomenological model in terms of flux tubes of flux amounts ≈ 10/sup17 − 10/sup18.5 Mx rising across the inner corona in the form of arches and opening out in the outer corona. In contrast to Parker’s estimate, this model is consistent with the observed spans of the chromospheric fibrils and x-ray arches. It is also consistent with the number of flux tubes present above the photosphere as estimated from the observed abundance of spicules.	en
dc.language.iso	en	en
dc.publisher	Indian Academy of Sciences	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1978Prama..11..547G	en
dc.relation.uri	http://www.springerlink.com/content/470n455t64570071/	en
dc.relation.uri	http://www.ias.ac.in/j_archive/pramana/11/vol11contents.html	en
dc.subject	Solar corona	en
dc.subject	Solar magnetic fields	en
dc.title	A phenomenological, kinematical model of the coronal magnetic fields in terms of thin flux tubes rising from the photosphere	en
dc.type	Article	en