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Solar Physics

, 294:152 | Cite as

Chromospheric Synoptic Maps of Polar Crown Filaments

  • A. DierckeEmail author
  • C. Denker
Article
Part of the following topical collections:
  1. Irradiance Variations of the Sun and Sun-like Stars

Abstract

Polar crown filaments form above the polarity inversion line between the old magnetic flux of the previous cycle and the new magnetic flux of the current cycle. Studying their appearance and their properties can lead to a better understanding of the solar cycle. We use full-disk data of the Chromospheric Telescope (ChroTel) at the Observatorio del Teide, Tenerife, Spain, which were taken in three different chromospheric absorption lines (H\(\upalpha\)\(\lambda\)6563 Å, Ca ii K \(\lambda\)3933 Å, and He i \(\lambda\)10830 Å), and we create synoptic maps. In addition, the spectroscopic He i data allow us to compute Doppler velocities and to create synoptic Doppler maps. ChroTel data cover the rising and decaying phase of Solar Cycle 24 on about 1000 days between 2012 and 2018. Based on these data, we automatically extract polar crown filaments with image-processing tools and study their properties. We compare contrast maps of polar crown filaments with those of quiet-Sun filaments. Furthermore, we present a super-synoptic map summarizing the entire ChroTel database. In summary, we provide statistical properties, i.e. number and location of filaments, area, and tilt angle for both the maximum and the declining phase of Solar Cycle 24. This demonstrates that ChroTel provides a promising data set to study the solar cycle.

Keywords

Chromosphere, quiet Prominences, quiescent Prominences, magnetic field Solar Cycle, observations Instrumentation and data management 

Notes

Acknowledgments

The Chromospheric Telescope (ChroTel) is operated by the Leibniz Institute for Solar Physics (KIS) in Freiburg, Germany, at the Spanish Observatorio del Teide on Tenerife (Spain). The ChroTel filtergraph was developed by KIS in cooperation with the High Altitude Observatory (HAO) in Boulder, Colorado. This study was supported by grant DE 787/5-1 of the Deutsche Forschungsgemeinschaft (DFG) and by the European Commission’s Horizon 2020 Program under grant agreements 824064 (ESCAPE – European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures) and 824135 (SOLARNET – Integrating High Resolution Solar Physics). A. Diercke thanks Christoph Kuckein, Stefan Hofmeister, and Ioannis Kontogiannis for their helpful comments. The authors thank the reviewer for constructive criticism and helpful suggestions improving the manuscript.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.Leibniz-Institut für Astrophysik Potsdam (AIP)PotsdamGermany
  2. 2.Institut für Physik und AstronomieUniversität PotsdamPotsdamGermany

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