Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7940
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dc.contributor.authorPrabhakar, Maya-
dc.contributor.authorRaju, K. P-
dc.date.accessioned2022-06-02T09:08:59Z-
dc.date.available2022-06-02T09:08:59Z-
dc.date.issued2022-05-20-
dc.identifier.citationThe Astrophysical Journal, Vol. 931, No. 1, 12en_US
dc.identifier.issn1538-4357-
dc.identifier.urihttp://hdl.handle.net/2248/7940-
dc.descriptionOpen Accessen_US
dc.descriptionOriginal 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.abstractCoronal active regions are studied using Hinode/EIS observations in the EUV line Fe xii λ195.12 by analyzing their line profiles from 2006 December to 2019 December. The period covers the last 2 yr of solar cycle 23 and solar cycle 24 fully. Active regions are the main source of magnetic field in the solar atmosphere, important in its heating and dynamics. Line profiles were obtained from various active regions spread across the Sun on a monthly basis from which we obtained the intensity, line width, Doppler velocity, and centroid and examined their variation during the solar cycle. The histograms of the Doppler velocity and centroid show that they behave in six different ways with respect to the position of rest wavelength. In addition, the shifts in the centroid were found to be more compared to the Doppler velocity. The variation of the line width with respect to the Doppler velocity or the centroid mostly follows a second-degree polynomial. A multicomponent line profile is simulated to explain the difference in the behavior of the Doppler velocity and the centroid with respect to the line width. We also find that the intensity and the line width of the different data sets show a global dependence on the solar cycle with a good correlation. The implications of the results for the coronal heating and dynamics are pointed out.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ac610e-
dc.rights© 2022. The Author(s)-
dc.subjectSolar atmosphereen_US
dc.subjectSolar coronaen_US
dc.subjectSolar active regionsen_US
dc.titleLine Profile Studies of Coronal Active Regions in Fe XII λ195.12 Using Hinode/EISen_US
dc.typeArticleen_US
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