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Equator to Pole Solar Chromospheric Differential Rotation Using Ca-K Features Derived from Kodaikanal Data

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dc.contributor.author Kharayat, Hema
dc.contributor.author Singh, J
dc.contributor.author Priyal, M
dc.contributor.author Ravindra, B
dc.date.accessioned 2024-06-28T08:49:49Z
dc.date.available 2024-06-28T08:49:49Z
dc.date.issued 2024-06-20
dc.identifier.citation The Astrophysical Journal, Vol. 968, No. 2, 53 en_US
dc.identifier.issn 1538-4357
dc.identifier.uri http://hdl.handle.net/2248/8495
dc.description Open Access. en_US
dc.description Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
dc.description.abstract Differential rotation is one of the basic characteristics of the Sun, and it plays an important role in generating the magnetic fields and its activities. We investigated rotation rate using chromospheric features such as plages, enhanced network (EN), active network (AN), and quiet network (QN) separately (for the first time). The digitized Ca-K images from Kodaikanal Observatory for 1907–1996 are used to study rotation over 0°–80° latitudes at an interval of 10°. We find that plages and all types of networks exhibit the differential rotation of the chromosphere. Furthermore, the rotation rate shows a decreasing pattern as one move from the equator to the higher polar latitudes for all the features used in the study. At the equator the rotation rate (rotation period) is obtained to be ∼13.98° day−1 (25.74 days), ∼13.91° day−1 (25.88 days), ∼13.99° day−1 (25.74 days), and ∼14.11° day−1 (25.51 days) for plage, EN, AN, and QN areas, respectively. By analyzing how the area of chromospheric features varies over time, we can effectively map the Sun’s rotation rate at all latitudes, including the polar regions. Interestingly, both plages and small-scale networks exhibit a similar differential rotation rate. This suggests these features likely rooted at the same layer below the visible surface of the Sun. Therefore, the long-term Ca-K data is very useful for studying the solar rotation rate at all latitudes including the polar regions. en_US
dc.language.iso en en_US
dc.publisher American Astronomical Society en_US
dc.relation.uri https://doi.org/10.3847/1538-4357/ad4992
dc.rights © 2024. The Author(s)
dc.subject Solar chromosphere en_US
dc.subject Plages en_US
dc.subject Solar rotation en_US
dc.subject Solar differential rotation en_US
dc.title Equator to Pole Solar Chromospheric Differential Rotation Using Ca-K Features Derived from Kodaikanal Data en_US
dc.type Article en_US


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