Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode
Low- m inertial modes have been recently discovered in the Sun’s high-latitude regions. In this study, we characterize the observational properties of the m = 1 mode by analyzing time–distance subsurface flow maps. Synoptic flow maps, constructed from daily subsurface flow maps using a tracking rate...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ade980 |
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| author | Boyang Ding Junwei Zhao Ruizhu Chen Matthias Waidele Sushant S. Mahajan Oana Vesa |
| author_facet | Boyang Ding Junwei Zhao Ruizhu Chen Matthias Waidele Sushant S. Mahajan Oana Vesa |
| author_sort | Boyang Ding |
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| description | Low- m inertial modes have been recently discovered in the Sun’s high-latitude regions. In this study, we characterize the observational properties of the m = 1 mode by analyzing time–distance subsurface flow maps. Synoptic flow maps, constructed from daily subsurface flow maps using a tracking rate corresponding to the rotation at latitude 65°, are filtered in both the spherical harmonic and Fourier domains to retain only the m = 1 mode and its dominant frequencies. Our analysis reveals a power distribution that is significantly stronger in the northern polar region. The mode’s power exhibits an anticorrelation with solar activity, remaining strong and persistent during the solar activity minimum and becoming weaker and more fragmented during the solar maximum. Magnetic flux transported from low to high latitudes influences both the mode’s power and lifetime, enhancing its power and shortening its lifetime upon arrival. The phases of the m = 1 mode in the northern and southern polar regions are near-antisymmetric for most of the time with short deviations. We also compute zonal and meridional phase velocities of the mode and find that it exhibits significantly less differential rotation than its surrounding plasma. The meridional phase velocity, comprising both the local plasma’s meridional flow and the mode’s intrinsic phase motion, is directed poleward below latitude 70° and equatorward above this latitude. These observational findings underscore the need for a deeper understanding of the internal dynamics of the low- m modes, which may offer valuable insights into the structure and dynamics of the solar interior. |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-db531bf4a21347f7b56435e738b31c9a2025-08-01T05:24:44ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198912610.3847/1538-4357/ade980Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial ModeBoyang Ding0https://orcid.org/0009-0001-5405-4042Junwei Zhao1https://orcid.org/0000-0002-6308-872XRuizhu Chen2https://orcid.org/0000-0002-2632-130XMatthias Waidele3https://orcid.org/0000-0003-2678-626XSushant S. Mahajan4https://orcid.org/0000-0003-1753-8002Oana Vesa5https://orcid.org/0000-0001-6754-1520Department of Physics, Stanford University , Stanford, CA 94305-4013, USA; W. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USAW. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USAW. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USAW. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USAW. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USAW. W. Hansen Experimental Physics Laboratory, Stanford University , Stanford, CA 94305-4085, USALow- m inertial modes have been recently discovered in the Sun’s high-latitude regions. In this study, we characterize the observational properties of the m = 1 mode by analyzing time–distance subsurface flow maps. Synoptic flow maps, constructed from daily subsurface flow maps using a tracking rate corresponding to the rotation at latitude 65°, are filtered in both the spherical harmonic and Fourier domains to retain only the m = 1 mode and its dominant frequencies. Our analysis reveals a power distribution that is significantly stronger in the northern polar region. The mode’s power exhibits an anticorrelation with solar activity, remaining strong and persistent during the solar activity minimum and becoming weaker and more fragmented during the solar maximum. Magnetic flux transported from low to high latitudes influences both the mode’s power and lifetime, enhancing its power and shortening its lifetime upon arrival. The phases of the m = 1 mode in the northern and southern polar regions are near-antisymmetric for most of the time with short deviations. We also compute zonal and meridional phase velocities of the mode and find that it exhibits significantly less differential rotation than its surrounding plasma. The meridional phase velocity, comprising both the local plasma’s meridional flow and the mode’s intrinsic phase motion, is directed poleward below latitude 70° and equatorward above this latitude. These observational findings underscore the need for a deeper understanding of the internal dynamics of the low- m modes, which may offer valuable insights into the structure and dynamics of the solar interior.https://doi.org/10.3847/1538-4357/ade980Solar interiorSolar oscillationsHelioseismologySolar rotation |
| spellingShingle | Boyang Ding Junwei Zhao Ruizhu Chen Matthias Waidele Sushant S. Mahajan Oana Vesa Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode The Astrophysical Journal Solar interior Solar oscillations Helioseismology Solar rotation |
| title | Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode |
| title_full | Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode |
| title_fullStr | Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode |
| title_full_unstemmed | Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode |
| title_short | Characterizing the Observational Properties of the Sun’s High-latitude m = 1 Inertial Mode |
| title_sort | characterizing the observational properties of the sun s high latitude m 1 inertial mode |
| topic | Solar interior Solar oscillations Helioseismology Solar rotation |
| url | https://doi.org/10.3847/1538-4357/ade980 |
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