Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5705
Title: Dynamic responses of sunspots to their ambient magnetic configuration
Authors: Bagare, S. P
Keywords: Photosphere;Sunspots;Magnetic fields
Issue Date: Aug-2011
Publisher: Cambridge University Press
Citation: The Physics of Sun and Star Spots, Proceedings of the International Astronomical Union, IAU Symposium, Vol. 273, pp. 308-314
Series/Report no.: International Astronomical Union Symposium; No. 273
Abstract: In our earlier study of a revisit of the classic Wilson Effect, it was found that a large proportion of sunspots do not display the geometric effect which is ascribed to a depression of the umbra. It was shown that the presence or absence of the effect, observed close to the limb, depends upon the ambient magnetic configuration of the sunspot. In this follow up study, we look for the impact of changes in ambient magnetic configuration on the measurable properties of sunspots during their disk passage, using observations obtained at the Kodaikanal observatory during 1978-80. Digitized photoheliogram data were used to examine and measure areas of spots and their umbrae for 101 cases. Magnetic field measures published by the Academy of sciences, Leningrad were used to evaluate the ambient magnetic configuration. The results indicate that the extent of magnetic bipolarity is associated with changes in the proportion of the area of the penumbra to that of the umbra. In regular spots, the relative area of penumbra reduces with reduction in the strength of ambient opposite polarity spots and pores. However, in the presence of pore sized blob(s) in penumbra, and with associated emerging fluxes, the penumbra is significantly enlarged. But in the presence of a light bridge or a split umbra, the relative area of penumbra is considerably reduced.
Description: Open Access
URI: http://hdl.handle.net/2248/5705
???metadata.dc.rights???: © International Astronomical Union
???metadata.dc.relation.uri???: http://dx.doi.org/10.1017/S1743921311015432
Appears in Collections:IIAP Publications

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