Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-25T18:46:02.607Z Has data issue: false hasContentIssue false
  • English
  • Français

Exploring Damping Properties of IRIS Bright Points using Deep Learning Techniques

Published online by Cambridge University Press:  23 December 2024

E. Tavabi Open the ORCID record for E. Tavabi [Opens in a new window]  and
R. Sadeghi Open the ORCID record for R. Sadeghi [Opens in a new window]
E. Tavabi*
Affiliation:
Physics Department, Payame Noor University, Tehran, Iran, 19395-3697
R. Sadeghi
Affiliation:
Physics Department, Payame Noor University, Tehran, Iran, 19395-3697
*
email: e_tavabi@pnu.ac.ir
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

This study analyzed the Doppler shift in the solar spectrum using the Interface Region Imaging Spectrograph (IRIS). Two types of oscillations were investigated: long period damp and short period damp. The researchers observed periodic perturbations in the Doppler velocity oscillations of bright points (BPs) in the chromosphere and transition region (TR). Deep learning techniques were used to examine the statistical properties of damping in different solar regions. The results showed variations in damping rates, with higher damping in coronal hole areas. The study provided insights into the damping behavior of BPs and contributed to our understanding of energy dissipation processes in the solar chromosphere and TR.

Keywords

deep learningbright pointsoscillationDoppler velocity
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. 399 - 403
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Ajabshirizadeh, A., Tavabi, E., & Koutchmy, S. L. Oscillation of ca h jet emission observed by sot: Viscous effects 2011,.Google Scholar
Chandrashekhar, K. & Sarkar, A. 2015, Modeling solar coronal bright-point oscillations with multiple nanoflare heated loops. The Astrophysical Journal, 810.Google Scholar
Krijger, J. M., Rutten, R. J., Lites, B. W., Straus, T., Shine, R. A., & Tarbell, T. D. 2001, Dynamics of the solar chromosphere - iii. ultraviolet brightness oscillations from trace. Astronomy and Astrophysics, 379, 1052–1082.CrossRefGoogle Scholar
Rojas–Quesada. Analysis of oscillations of thequiescent solar filaments 2021,.Google Scholar
Sadeghi, R. & Tavabi, E. 2022,a Characteristics of chromospheric oscillation periods in magnetic bright points (mbps). Monthly Notices of the Royal Astronomical Society,.CrossRefGoogle Scholar
Sadeghi, R. & Tavabi, E. 2022,b A new approach to kinetic energy flux at the different frequencies above the iris bright points. The Astrophysical Journal, 938b.CrossRefGoogle Scholar
Tavabi, E. 2018, Synchronized observations of bright points from the solar photosphere to the corona. Monthly Notices of the Royal Astronomical Society, 476, 868–874.CrossRefGoogle Scholar
Tavabi, E., Koutchmy, S. L., Ajabshirizadeh, A., Zhelyazkov, I., & Mishonov, T. M. Null-point oscillations of chromospheric large cool jets 2011,.CrossRefGoogle Scholar
Tavabi, E., Koutchmy, S. L., & Golub, L. 2015, Limb event brightenings and fast ejection using iris mission observations. Solar Physics, 290, 2871–2887.CrossRefGoogle Scholar
Tavabi, E., Zeighami, S., & Heydari, M. 2022, Dynamics of explosive events observed by the interface region imaging spectrograph. Solar Physics, 297.Google Scholar
Zeighami, S., Tavabi, E., & Amirkhanlou, E. 2020, Waves propagation in network and inter-network bright points channels between the chromosphere and transition regions with iris observations. Journal of Astrophysics and Astronomy, 41, 1–14.CrossRefGoogle Scholar