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Analyzing Magnetic Network and its Variations over Solar Cycles 23, 24 and 25 Based on Magnetic Power Spectra

Published online by Cambridge University Press:  23 December 2024

Yukun Luo Open the ORCID record for Yukun Luo [Opens in a new window] ,
Jie Jiang Open the ORCID record for Jie Jiang [Opens in a new window]  and
Ruihui Wang Open the ORCID record for Ruihui Wang [Opens in a new window]
Yukun Luo*
Affiliation:
School of Space and Environment, Beihang University, Beijing, China Key Laboratory of Space Environment monitoring and Information Processing of MIIT, Beijing, China
Jie Jiang
Affiliation:
School of Space and Environment, Beihang University, Beijing, China Key Laboratory of Space Environment monitoring and Information Processing of MIIT, Beijing, China
Ruihui Wang
Affiliation:
School of Space and Environment, Beihang University, Beijing, China Key Laboratory of Space Environment monitoring and Information Processing of MIIT, Beijing, China
*
email: [email protected]
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Abstract

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The magnetic network is a typical magnetic structure of the quiet Sun. Investigating its cycle dependence is crucial for understanding its evolution. We aim to identify and analyze the spatial scales of the magnetic network within magnetic power spectra derived from high-resolution Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) and Solar Dynamics Observatory (SDO)/ Helioseismic and Magnetic Imager (HMI) synoptic magnetograms. The data sets cover the entirety of solar cycles 23, 24, and part of cycle 25. We find that the identified magnetic network sizes identified range from 26 Mm to 41 Mm. There seems to be no obvious dependence on the solar cycle, and the sizes are distributed uniformly within the identification range.

Keywords

Magnetic Network SizeSolar Cycle Dependence
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 19 - 23
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Bellot Rubio, L. & Orozco Suárez, D. 2019, Quiet Sun magnetic fields: an observational view. Living Reviews in Solar Physics, 16(1), 1.CrossRefGoogle Scholar
Berrilli, F., Ermolli, I., Florio, A., & Pietropaolo, E. 1999, Average properties and temporal variations of the geometry of solar network cells. Astron. Astrophys., 344, 965–972.Google Scholar
Gosic, M. 2015,. The solar internetwork. PhD thesis, University of Granada, Spain.Google Scholar
Hagenaar, H. J., Schrijver, C. J., & Title, A. M. 1997, The Distribution of Cell Sizes of the Solar Chromospheric Network. Astrophys. J., 481(2), 988–995.CrossRefGoogle Scholar
Hagenaar, H. J., Schrijver, C. J., & Title, A. M. 2003, The Properties of Small Magnetic Regions on the Solar Surface and the Implications for the Solar Dynamo(s). Astrophys. J., 584(2), 1107–1119.CrossRefGoogle Scholar
Luo, Y., Jiang, J., & Wang, R. 2023, The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms. Astrophys. J., 954(2), 199.CrossRefGoogle Scholar
Luo, Y., Jiang, J., & Wang, R. 2024, The Sun’s Magnetic Power Spectra over Two Solar Cycles. II. Cycle Dependence of Active Region and Magnetic Network. in Prep.,.CrossRefGoogle Scholar
Muenzer, H., Schroeter, E. H., Woehl, H., & Hanslmeier, A. 1989, Pole-equator-difference of the size of the chromospheric CA II-K-network in quiet and active solar regions. Astron. Astrophys., 213(1-2), 431–435.Google Scholar
Rincon, F. & Rieutord, M. 2018, The Sun’s supergranulation. Living Reviews in Solar Physics, 15(1), 6.CrossRefGoogle Scholar
Simon, G. W. & Leighton, R. B. 1964, Velocity Fields in the Solar Atmosphere. III. Large-Scale Motions, the Chromospheric Network, and Magnetic Fields. Astrophys. J., 140, 1120.CrossRefGoogle Scholar
Singh, J. & Bappu, M. K. V. 1981, A dependence on solar cycle of the size of the CA+ network. Solar Phys., 71(1), 161–168.CrossRefGoogle Scholar
Solanki, S. K., Krivova, N. A., & Haigh, J. D. 2013, Solar Irradiance Variability and Climate. ARA&A, 51(1), 311–351.Google Scholar