Analysis of full-disc Hα observations: Carrington maps and filament properties in 1909–2022^⋆

¹ Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
e-mail: chatzistergos@mps.mpg.de
² INAF Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monte Porzio Catone, Italy
³ Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263 001, India
⁴ Instituto de Astrofísica e Ciências do Espaço, University of Coimbra, R. do Observatório, 3040-004 Coimbra, Portugal
⁵ Department of Earth Sciences, University of Coimbra, R. Sílvio Lima, 3030-790 Coimbra, Portugal
⁶ Larissa Observatory “Aristeus”, Giannouli, 41500 Larissa, Greece
⁷ INAF Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
⁸ Department of Physics, University of Coimbra, R. Larga, 3004-516 Coimbra, Portugal
⁹ National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
¹⁰ Astronomical Institute of Kharkiv V.N. Karazin National University, 35 Sumskaya St., Kharkiv 61022, Ukraine
¹¹ LESIA, Observatoire de Paris, 5 Pl. Jules Janssen, 92195 Meudon, France
¹² PSL Research University, 60 Rue Mazarine, 75006 Paris, France

Received: 22 July 2023
Accepted: 16 September 2023

Abstract

Context. Full-disc observations of the Sun in the Hα line provide information about the solar chromosphere, and in particular, about the filaments, which are dark and elongated features that lie along magnetic field polarity-inversion lines. This makes them important for studies of solar magnetism. Because full-disc Hα observations have been performed at various sites since the second half of the 19th century, with regular photographic data having started at the beginning of the 20th century, they are an invaluable source of information on past solar magnetism.

Aims. We derive accurate information about filaments from historical and modern full-disc Hα observations.

Methods. We consistently processed observations from 15 Hα archives spanning 1909–2022. The analysed datasets include long-running ones such as those from Meudon and Kodaikanal, but also previously unexplored datasets such as those from Arcetri, Boulder, Larissa, and Upice. Our data processing includes photometric calibration of the data stored on photographic plates, the compensation for limb-darkening, and the orientation of the data to align solar north at the top of the images. We also constructed Carrington maps from the calibrated Hα images.

Results. We find that filament areas, similar to plage areas in Ca II K data, are affected by the bandwidth of the observation. Thus, a cross calibration of the filament areas derived from different archives is needed. We produced a composite of filament areas from individual archives by scaling all of them to the Meudon series. Our composite butterfly diagram very distinctly shows the common features of filament evolution, that is, the poleward migration as well as a decrease in the mean latitude of filaments as the cycle progresses. We also find that during activity maxima, filaments cover ∼1% of the solar surface on average. The change in the amplitude of cycles in filament areas is weaker than in sunspot and plage areas.

Conclusions. Analysis of Hα data for archives with contemporaneous Ca II K observations allowed us to identify and verify archive inconsistencies, which also have implications for reconstructions of past solar magnetism and irradiance from Ca II K data.