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Characterizing Solar Spicules and their Role in Solar Wind Production using Machine Learning and the Hough Transform

Published online by Cambridge University Press:  23 December 2024

R. Sadeghi Open the ORCID record for R. Sadeghi [Opens in a new window]  and
E. Tavabi Open the ORCID record for E. Tavabi [Opens in a new window]
R. Sadeghi
Affiliation:
Physics Department, Payame Noor University, Tehran, Iran, 19395-3697
E. Tavabi*
Affiliation:
Physics Department, Payame Noor University, Tehran, Iran, 19395-3697
*
email: [email protected]
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Abstract

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Solar winds originate from the Sun and can be classified as fast or slow. Fast solar winds come from coronal holes at the solar poles, while slow solar winds may originate from the equatorial region or streamers. Spicules are jet-like structures observed in the Sun’s chromosphere and transition region. Some spicules exhibit rotating motion, potentially indicating vorticity and Alfvén waves. Machine learning and the Hough algorithm were used to analyze over 3000 frames of the Sun, identifying spicules and their characteristics. The study found that rotating spicules, accounting for 21% at the poles and 4% at the equator, play a role in energy transfer to the upper solar atmosphere. The observations suggest connections between spicules, mini-loops, magnetic reconnection, and the acceleration of fast solar winds. Understanding these small-scale structures is crucial for comprehending the origin and heating of the fast solar wind.

Keywords

Spiculesolar windmachine learningHough Transform
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. 394 - 398
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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