{"title":"太阳周期 23 至 25 的地表下流动的长期趋势","authors":"Rudolf Komm","doi":"10.1007/s11207-024-02397-6","DOIUrl":null,"url":null,"abstract":"<div><p>We study the long-term variation of the zonal and meridional flows from Solar Cycle 23 to 25 derived with ring-diagram analysis applied to <i>Global Oscillation Network Group</i> (GONG) and <i>Helioseismic and Magnetic Imager</i> (HMI) Dopplergrams. We focus mainly on the subsurface flows averaged over depths from 2.0 Mm to 11.6 Mm since their long-term variations are sufficiently similar. First, we examine their temporal variations for systematic artifacts. We find that the GONG-derived zonal flows increase almost linearly with time until about 2020, which we correct with a linear regression. Then we determine the average differences between the GONG- and HMI-derived flows. The average offset is <span>\\(0.15 \\pm 0.53\\)</span> m s<sup>−1</sup> for the zonal flow and <span>\\(0.65 \\pm 0.08\\)</span> m s<sup>−1</sup> for the meridional flow within <span>\\(\\pm 30.0^{\\circ }\\)</span> latitude. The average difference of the meridional flow is nearly constant with latitude in this range, whereas that of the zonal flow varies similarly to that of the magnetic activity. At latitudes of 45.0<sup>∘</sup> and higher, the differences increase and are larger than those at lower latitudes, which is most likely due to the combined effect of different spatial resolution between GONG and HMI and geometric projection effects. Finally, we combine the GONG- and HMI-derived flows and find, as expected, that the solar-cycle variation is the dominant long-term variation. At each latitude within <span>\\(\\pm 30.0^{\\circ }\\)</span>, the meridional-flow pattern appears ahead of the zonal-flow pattern by an average lag of <span>\\(0.926 \\pm 0.126\\)</span> years. The equatorward and poleward branches of the solar-cycle variation occur at 52.5<sup>∘</sup> with the poleward branches present near 60.0<sup>∘</sup> and the equatorward ones at lower latitudes. The zonal flows at 52.5<sup>∘</sup> and 60.0<sup>∘</sup> show an additional trend and decrease by <span>\\(2.9 \\pm 0. 3\\)</span> m s<sup>−1</sup> over 11 years. This decrease might nevertheless be related to the solar cycle and imply that the flow amplitudes are anticorrelated with the strength of the associated solar cycle.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 10","pages":""},"PeriodicalIF":2.7000,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Long-Term Trends in Subsurface Flows of Solar Cycle 23 to 25\",\"authors\":\"Rudolf Komm\",\"doi\":\"10.1007/s11207-024-02397-6\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>We study the long-term variation of the zonal and meridional flows from Solar Cycle 23 to 25 derived with ring-diagram analysis applied to <i>Global Oscillation Network Group</i> (GONG) and <i>Helioseismic and Magnetic Imager</i> (HMI) Dopplergrams. We focus mainly on the subsurface flows averaged over depths from 2.0 Mm to 11.6 Mm since their long-term variations are sufficiently similar. First, we examine their temporal variations for systematic artifacts. We find that the GONG-derived zonal flows increase almost linearly with time until about 2020, which we correct with a linear regression. Then we determine the average differences between the GONG- and HMI-derived flows. The average offset is <span>\\\\(0.15 \\\\pm 0.53\\\\)</span> m s<sup>−1</sup> for the zonal flow and <span>\\\\(0.65 \\\\pm 0.08\\\\)</span> m s<sup>−1</sup> for the meridional flow within <span>\\\\(\\\\pm 30.0^{\\\\circ }\\\\)</span> latitude. The average difference of the meridional flow is nearly constant with latitude in this range, whereas that of the zonal flow varies similarly to that of the magnetic activity. At latitudes of 45.0<sup>∘</sup> and higher, the differences increase and are larger than those at lower latitudes, which is most likely due to the combined effect of different spatial resolution between GONG and HMI and geometric projection effects. Finally, we combine the GONG- and HMI-derived flows and find, as expected, that the solar-cycle variation is the dominant long-term variation. At each latitude within <span>\\\\(\\\\pm 30.0^{\\\\circ }\\\\)</span>, the meridional-flow pattern appears ahead of the zonal-flow pattern by an average lag of <span>\\\\(0.926 \\\\pm 0.126\\\\)</span> years. The equatorward and poleward branches of the solar-cycle variation occur at 52.5<sup>∘</sup> with the poleward branches present near 60.0<sup>∘</sup> and the equatorward ones at lower latitudes. The zonal flows at 52.5<sup>∘</sup> and 60.0<sup>∘</sup> show an additional trend and decrease by <span>\\\\(2.9 \\\\pm 0. 3\\\\)</span> m s<sup>−1</sup> over 11 years. This decrease might nevertheless be related to the solar cycle and imply that the flow amplitudes are anticorrelated with the strength of the associated solar cycle.</p></div>\",\"PeriodicalId\":777,\"journal\":{\"name\":\"Solar Physics\",\"volume\":\"299 10\",\"pages\":\"\"},\"PeriodicalIF\":2.7000,\"publicationDate\":\"2024-10-25\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Solar Physics\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://link.springer.com/article/10.1007/s11207-024-02397-6\",\"RegionNum\":3,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Solar Physics","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s11207-024-02397-6","RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0
摘要
我们研究了太阳周期 23 至 25 的纵向和经向流的长期变化,这些变化是通过对全球涛动网络组(GONG)和日震与磁成像仪(HMI)多普勒图进行环图分析得出的。我们主要关注的是平均深度为 2.0 毫米到 11.6 毫米的次表层流,因为它们的长期变化非常相似。首先,我们研究了它们的时间变化,以寻找系统性伪影。我们发现,在 2020 年之前,由 GONG 得出的带状流几乎随时间呈线性增长,我们对此进行了线性回归校正。然后,我们确定 GONG 和 HMI 导出流量之间的平均差异。在 30.0^{/circ }纬度范围内,经向流的平均偏移量为 0.65 m s-1。在这一范围内,经向流的平均差值随纬度的变化几乎是恒定的,而带流的平均差值与磁活动的平均差值变化相似。在纬度 45.0∘及更高的纬度上,差异增大,而且比低纬度上的差异更大,这很可能是由于 GONG 和 HMI 的空间分辨率不同以及几何投影效应的综合影响。最后,我们综合了 GONG 和 HMI 得出的流量,发现正如预期的那样,太阳周期变化是主要的长期变化。在每个纬度(30.0^/pm)范围内,经向流模式比纬向流模式平均滞后(0.926/pm 0.126)年。太阳周期变化的赤道分支和极地分支出现在52.5∘,极地分支出现在60.0∘附近,赤道分支出现在较低纬度。52.5∘和60.0∘处的带状流显示出一种额外的趋势,在11年中减少了(2.9\pm 0. 3\) m s-1。然而,这种下降可能与太阳周期有关,并意味着流动振幅与相关太阳周期的强度是反相关的。
Long-Term Trends in Subsurface Flows of Solar Cycle 23 to 25
We study the long-term variation of the zonal and meridional flows from Solar Cycle 23 to 25 derived with ring-diagram analysis applied to Global Oscillation Network Group (GONG) and Helioseismic and Magnetic Imager (HMI) Dopplergrams. We focus mainly on the subsurface flows averaged over depths from 2.0 Mm to 11.6 Mm since their long-term variations are sufficiently similar. First, we examine their temporal variations for systematic artifacts. We find that the GONG-derived zonal flows increase almost linearly with time until about 2020, which we correct with a linear regression. Then we determine the average differences between the GONG- and HMI-derived flows. The average offset is \(0.15 \pm 0.53\) m s−1 for the zonal flow and \(0.65 \pm 0.08\) m s−1 for the meridional flow within \(\pm 30.0^{\circ }\) latitude. The average difference of the meridional flow is nearly constant with latitude in this range, whereas that of the zonal flow varies similarly to that of the magnetic activity. At latitudes of 45.0∘ and higher, the differences increase and are larger than those at lower latitudes, which is most likely due to the combined effect of different spatial resolution between GONG and HMI and geometric projection effects. Finally, we combine the GONG- and HMI-derived flows and find, as expected, that the solar-cycle variation is the dominant long-term variation. At each latitude within \(\pm 30.0^{\circ }\), the meridional-flow pattern appears ahead of the zonal-flow pattern by an average lag of \(0.926 \pm 0.126\) years. The equatorward and poleward branches of the solar-cycle variation occur at 52.5∘ with the poleward branches present near 60.0∘ and the equatorward ones at lower latitudes. The zonal flows at 52.5∘ and 60.0∘ show an additional trend and decrease by \(2.9 \pm 0. 3\) m s−1 over 11 years. This decrease might nevertheless be related to the solar cycle and imply that the flow amplitudes are anticorrelated with the strength of the associated solar cycle.
期刊介绍:
Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.