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Temporal Variation of Solar Equatorial Rossby Modes with Azimuthal Orders 6 ≤ m ≤ 10

Published online by Cambridge University Press:  23 December 2024

B. Lekshmi Open the ORCID record for B. Lekshmi [Opens in a new window] ,
Laurent Gizon Open the ORCID record for Laurent Gizon [Opens in a new window] ,
Kiran Jain Open the ORCID record for Kiran Jain [Opens in a new window] ,
Zhi–Chao Liang Open the ORCID record for Zhi–Chao Liang [Opens in a new window]  and
Jordan Philidet Open the ORCID record for Jordan Philidet [Opens in a new window]
B. Lekshmi*
Affiliation:
Max–Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
Laurent Gizon
Affiliation:
Max–Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany Institut für Astrophysik, Georg–August-Universität Göttingen, 37077 Göttingen, Germany
Kiran Jain
Affiliation:
National Solar Observatory, Boulder, CO 80303, USA
Zhi–Chao Liang
Affiliation:
Max–Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
Jordan Philidet
Affiliation:
Max–Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
*
email: [email protected]
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Abstract

We use nearly two decades of helioseismic data obtained from the GONG (2002–2020) and HMI (2010–2020) ring-diagram pipelines to examine the temporal variations of the properties of individual equatorial Rossby modes with azimuthal orders in the range 6 ≤ m ≤ 10. We find that the mode parameters obtained from GONG and HMI are consistent during the data overlapping period of 2010–2020. The power and the frequency of each mode exhibit significant temporal variations over the full observing period. Using the GONG data during solar cycles 23 and 24, we find that the mode power averaged over 6 ≤ m ≤ 10 shows a positive correlation with the sunspot number (0.42), while the averaged frequency shift is anti-correlated (–0.91). The anti-correlation between the average mode power and frequency shift is –0.44.

Keywords

helioseismologysolar inertial modessunspot cycle
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. 230 - 234
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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References

Löptien, Björn & Gizon, Laurent & Birch, Aaron C. & Schou, Jesper & Proxauf, Bastian and Duvall, Thomas L. & Bogart, Richard S. & Christensen, Ulrich R., 2018, Nature Astronomy, 2, 568–573 CrossRefGoogle Scholar
Liang, Z.-C., Gizon, L., Birch, A. C., & Duvall, T. L. 2019, Time-distance helioseismology of solar Rossby waves Astron. Astrophys., 626, A3.CrossRefGoogle Scholar
Gizon, L., Cameron, R. H., Bekki, Y., Birch, A. C., Bogart, R. S., Brun, A. S., Damiani, C., Fournier, D., Hyest, L., Jain, K., Lekshmi, B., Liang, Z.-C., & Proxauf, B. 2021, Solar inertial modes: Observations, identification, and diagnostic promise. Astron. Astrophys., 652, L6.CrossRefGoogle Scholar
Hanson, C. S., Gizon, L., & Liang, Z.-C. 2020, Solar Rossby waves observed in GONG++ ring-diagram flow maps. Astron. Astrophys., 635, A109.CrossRefGoogle Scholar
Waidele, M. & Zhao, J. 2023, Observed power and frequency variations of solar rossby waves with solar cycles, Astrophys. J., 954, L26.CrossRefGoogle Scholar
Corbard, T., Toner, C., Hill, F., Hanna, K. D., Haber, D. A., Hindman, B. W., & Bogart, R. S. Ring-diagram analysis with GONG++. In Sawaya–Lacoste, H., editor, GONG+ 2002. Local and Global Helioseismology: the Present and Future 2003, Vol. 517, ESA Special Publication, pp. 255–258.Google Scholar
Bogart, R. S., Baldner, C., Basu, S., Haber, D. A., & Rabello–Soares, M. C. 2011, HMI ring diagram analysis I. The processing pipeline. J. Phys. Conf. Series, 271, 012008.CrossRefGoogle Scholar
Proxauf, B., Gizon, L., Löptien, B., Schou, J., Birch, A. C., & Bogart, R. S. 2020, Exploring the latitude and depth dependence of solar Rossby waves using ring-diagram analysis, Astron. Astrophys., 634, A44.CrossRefGoogle Scholar
SILSO, World Data Center - Sunspot Number and Long-term Solar Observations, Royal Observatory of Belgium, on-line Sunspot Number catalogue: http://www.sidc.be/SILSO/, 2002–2020Google Scholar
Goddard, C. R. and Birch, A. C. and Fournier, D. and Gizon, L. 2020, Predicting frequency changes of global-scale solar Rossby modes due to solar cycle changes in internal rotation, Astron. Astrophys., 640, L10.CrossRefGoogle Scholar