Volume 653, September 2021
|Number of page(s)||8|
|Section||The Sun and the Heliosphere|
|Published online||24 September 2021|
Rieger-type periodicity in the total irradiance of the Sun as a star during solar cycles 23–24
Georg-August-Universität, Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
2 School of Natural Sciences and Medicine, Ilia State University, Cholokashvili ave. 3/5, Tbilisi, Georgia
3 E.Kharadze Georgian National Astrophysical Observatory, Mount Kanobili, Georgia
4 Institute of Physics, IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
5 INAF-Osservatorio Astrofisico di Catania, Via S. Sofia, 78, 95123 Catania, Italy
6 Departament de Física & Institut d’Aplicacions Computacionals de Codi Comunitari (IAC3), Universitat de les Illes Balears, 07122 Palma de Mallorca, Spain
7 Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
Accepted: 28 July 2021
Context. Total solar irradiance allows for the use of the Sun as a star for studying observations of stellar light curves from recent space missions.
Aims. We aim to study how the mid-range periodicity observed in solar activity indices influences the total solar irradiance.
Methods. We studied periodic variations of total solar irradiance based on SATIRE-S and SOHO/VIRGO data during solar cycles 23–24 on timescales of Rieger-type periodicity. Then we compared the power spectrum of oscillations in the total solar irradiance to those of sunspot and faculae data to determine their contributions.
Results. Wavelet analyses of TSI data reveal strong peaks at 180 days and 115 days in cycle 23, while cycle 24 showed periods of 170 days and 145 days. There are several periods in the sunspot and faculae data that are not seen in total solar irradiance as they probably cancel each other out through simultaneous brightening (in faculae) and darkening (in sunspots). Rieger-type periodicity is probably caused by magneto-Rossby waves in the internal dynamo layer, where the solar cyclic magnetic field is generated. Therefore, the observed periods in the total solar irradiance and the wave dispersion relation allow us to estimate the dynamo magnetic field strength as 10–15 kG.
Conclusions. Total solar irradiance can be used to estimate the magnetic field strength in the dynamo layer. This tool can be of importance in estimating the dynamo magnetic field strength of solar-like stars using light curves obtained by space missions.
Key words: Sun: activity / Sun: magnetic fields / Sun: faculae, plages / sunspots
© ESO 2021
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