Meridional Movements of Individual Sunspots and Pores
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arXiv
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| Natura: | Preprint |
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2025
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| _version_ | 1866918074725171200 |
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| author | Tlatov, Andrey Tlatova, Kseniya |
| author_facet | Tlatov, Andrey Tlatova, Kseniya |
| contents | The analysis of the meridional displacement velocity of individual solar pores and sunspots has been performed. In the period May 2010\,-\,March 2025 of observations in the continuum of the \textit{Solar Dynamics Observatory/Helioseismic and Magnetic Imager} (SDO/HMI), we identified more than $3.6\cdot 10^{5}$ sunspots and pores for analysis and tracked their displacement. The velocity of the meridional displacement of spots $v_{\rm m}$ depends on their magnetic polarity, latitude, and stage of development. For sunspots and pores of trailing polarity, the velocity of movement is on average directed toward the poles. For such spots, the dependence of the velocity on latitude can be represented by linear regressions for pores: $v^{\rm pr}_{\rm tr} \approx 2.0+0.62\cdot θ^{\rm o}$ m s$^{-1}$; for sunspots: $v^{\rm sp}_{\rm tr}\approx 0.02+0.94\cdot θ^{\rm o}$ m s$^{-1}$. For sunspots and pores of leading polarity, the dependence is non-monotonic in nature on latitude. For pores: $v^{\rm pr}_{\rm ld}\approx 0.35-11.7\cdot {\rm sin}(θ)+16.5\cdot {\rm sin}^{\rm 2} (θ) +76.5\cdot {\rm sin}^3 (θ)-32.7\cdot {\rm sin}^{4}(θ)$ m s$^{-1}$; for sunspots: $v^{\rm sp}_{\rm ld}\approx -0.35-18.3\cdot {\rm sin}(θ)+32.2\cdot {\rm sin}^{\rm 2}(θ) +71.4\cdot {\rm sin}^{\rm 3} (θ)-6.7\cdot {\rm sin}^{\rm 4}(θ)$ m s$^{-1}$. The highest speed of meridional movement to the poles is observed for sunspots of trailing polarity during the phase of growth of the sunspot area. The velocity of the meridional movement depends on their area, reaching a maximum for an area of $S\approx 80 - 100$ $μ$sh. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_22751 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Meridional Movements of Individual Sunspots and Pores Tlatov, Andrey Tlatova, Kseniya Solar and Stellar Astrophysics The analysis of the meridional displacement velocity of individual solar pores and sunspots has been performed. In the period May 2010\,-\,March 2025 of observations in the continuum of the \textit{Solar Dynamics Observatory/Helioseismic and Magnetic Imager} (SDO/HMI), we identified more than $3.6\cdot 10^{5}$ sunspots and pores for analysis and tracked their displacement. The velocity of the meridional displacement of spots $v_{\rm m}$ depends on their magnetic polarity, latitude, and stage of development. For sunspots and pores of trailing polarity, the velocity of movement is on average directed toward the poles. For such spots, the dependence of the velocity on latitude can be represented by linear regressions for pores: $v^{\rm pr}_{\rm tr} \approx 2.0+0.62\cdot θ^{\rm o}$ m s$^{-1}$; for sunspots: $v^{\rm sp}_{\rm tr}\approx 0.02+0.94\cdot θ^{\rm o}$ m s$^{-1}$. For sunspots and pores of leading polarity, the dependence is non-monotonic in nature on latitude. For pores: $v^{\rm pr}_{\rm ld}\approx 0.35-11.7\cdot {\rm sin}(θ)+16.5\cdot {\rm sin}^{\rm 2} (θ) +76.5\cdot {\rm sin}^3 (θ)-32.7\cdot {\rm sin}^{4}(θ)$ m s$^{-1}$; for sunspots: $v^{\rm sp}_{\rm ld}\approx -0.35-18.3\cdot {\rm sin}(θ)+32.2\cdot {\rm sin}^{\rm 2}(θ) +71.4\cdot {\rm sin}^{\rm 3} (θ)-6.7\cdot {\rm sin}^{\rm 4}(θ)$ m s$^{-1}$. The highest speed of meridional movement to the poles is observed for sunspots of trailing polarity during the phase of growth of the sunspot area. The velocity of the meridional movement depends on their area, reaching a maximum for an area of $S\approx 80 - 100$ $μ$sh. |
| title | Meridional Movements of Individual Sunspots and Pores |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2506.22751 |