Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7290
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dc.contributor.authorPandey, K. K-
dc.contributor.authorHiremath, K. M-
dc.contributor.authorYellaiah, G-
dc.date.accessioned2020-11-19T14:01:21Z-
dc.date.available2020-11-19T14:01:21Z-
dc.date.issued2017-06-
dc.identifier.citationAstrophysics and Space Science, Vol. 362, 106en_US
dc.identifier.issn0004-640X-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/7290-
dc.descriptionRestricted Access The original publication is available at springerlink.com © Springer http://dx.doi.org/10.1007/s10509-017-3083-2en_US
dc.description.abstractThe time interval, between two highest peaks of the sunspot maximum, during which activity energy substantially absorbed is called Gnevyshev gap. In this study we focus on mysterious evolution of the Gnevyshev gap by analyzing and comparing the integrated (over the whole Sun) characteristics of magnetic field strength of sunspot groups, soft x-ray flares, filaments or prominences and polar faculae. The time latitude distribution of these solar activities from photosphere to coronal height, for the low (≤50∘) and high (≥50∘) latitudes, shows the way Gnevyshev gap is evolved. The presence of double peak structure is noticed in high latitude (≥50∘) activity. During activity maximum the depression (or valley) appearing, in different activity processes, probably due to shifting, spreading, and transfer of energy from higher to lower latitudes with the progress of solar cycle. The morphology of successive lower latitude zones, considering it as a wave pulse, appears to be modified/scattered, by certain degree due to shifting of magnetic energy to empower higher or lower latitudes.en_US
dc.language.isoenen_US
dc.publisherSpringeren_US
dc.subjectSun: higher latitude activityen_US
dc.subjectSun: lower latitude activityen_US
dc.titleLatitude character and evolution of Gnevyshev gapen_US
dc.typeArticleen_US
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