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p‐mode power variation with solar atmosphere as observed in the Na D1 and K spectral lines
Author(s) -
Simoniello R.,
JiménezReyes S.J.,
García R.A.,
Pallé P.L.
Publication year - 2008
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.200710983
Subject(s) - chromosphere , atmosphere (unit) , photosphere , spectral line , physics , line (geometry) , astrophysics , solar atmosphere , mode (computer interface) , span (engineering) , variation (astronomy) , atmospheric sciences , astronomy , meteorology , geometry , mathematics , civil engineering , quantum mechanics , magnetic field , computer science , engineering , operating system
In this work we investigate p‐mode power variation with solar atmosphere. To this aim, we use THÉMIS observations of the Na D1 ( λ 5896 Å) and K ( λ 7699 Å) spectral lines. While the formation heights of the K spectral line are essentially located in the photospheric layer, the formation heights of the Na D1 line span a much wider region: from photosphere up to chromosphere. Hence, we had the opportunity to infer p‐mode power variation up to the chromospheric layer. By analyzing power spectra obtained by temporal series at different points of the Na D1 and K spectral lines, we confirm and quantify the increase in p‐mode power towards higher atmospheric layers. Furthermore, the large span in formation heights of the Na D1 line induces a larger enhancement of p‐mode power with solar atmosphere compared to the K spectral line. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)