The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence
Solar wind dynamic pressure pulses (DPPs) are small-scale plasma structures with abrupt and large-amplitude plasma dynamic pressure changes on timescales of seconds to several minutes. Overwhelming majority of DPP events (around 79.13%) reside in large-scale solar wind transients, i.e., coronal mass...
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| Language: | English |
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Frontiers Media S.A.
2021-11-01
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| Series: | Frontiers in Physics |
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| Online Access: | https://www.frontiersin.org/articles/10.3389/fphy.2021.750410/full |
| _version_ | 1819199661800423424 |
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| author | Mengsi Ruan Pingbing Zuo Zilu Zhou Zhenning Shen Yi Wang Xueshang Feng Chaowei Jiang Xiaojun Xu Jiayun Wei Yanyan Xiong Ludi Wang |
| author_facet | Mengsi Ruan Pingbing Zuo Zilu Zhou Zhenning Shen Yi Wang Xueshang Feng Chaowei Jiang Xiaojun Xu Jiayun Wei Yanyan Xiong Ludi Wang |
| author_sort | Mengsi Ruan |
| collection | DOAJ |
| description | Solar wind dynamic pressure pulses (DPPs) are small-scale plasma structures with abrupt and large-amplitude plasma dynamic pressure changes on timescales of seconds to several minutes. Overwhelming majority of DPP events (around 79.13%) reside in large-scale solar wind transients, i.e., coronal mass ejections, stream interaction regions, and complex ejecta. In this study, the intermittency, which is a typical feature of solar wind turbulence, is determined and compared during the time intervals in the undisturbed solar wind and in large-scale solar wind transients with clustered DPP events, respectively, as well as in the undisturbed solar wind without DPPs. The probability distribution functions (PDFs) of the fluctuations of proton density increments normalized to the standard deviation at different time lags in the three types of distinct regions are calculated. The PDFs in the undisturbed solar wind without DPPs are near-Gaussian distributions. However, the PDFs in the solar wind with clustered DPPs are obviously non-Gaussian distributions, and the intermittency is much stronger in the large-scale solar wind transients than that in the undisturbed solar wind. The major components of the DPPs are tangential discontinuities (TDs) and rotational discontinuities (RDs), which are suggested to be formed by compressive magnetohydrodynamic (MHD) turbulence. There are far more TD-type DPPs than RD-type DPPs both in the undisturbed solar wind and large-scale solar wind transients. The results imply that the formation of solar wind DPPs could be associated with solar wind turbulence, and much stronger intermittency may be responsible for the high occurrence rate of DPPs in the large-scale solar wind transients. |
| first_indexed | 2024-12-23T03:19:53Z |
| format | Article |
| id | doaj.art-4d4b53f5a0b0486492cc4618ea4b7159 |
| institution | Directory Open Access Journal |
| issn | 2296-424X |
| language | English |
| last_indexed | 2024-12-23T03:19:53Z |
| publishDate | 2021-11-01 |
| publisher | Frontiers Media S.A. |
| record_format | Article |
| series | Frontiers in Physics |
| spelling | doaj.art-4d4b53f5a0b0486492cc4618ea4b71592022-12-21T18:02:02ZengFrontiers Media S.A.Frontiers in Physics2296-424X2021-11-01910.3389/fphy.2021.750410750410The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind TurbulenceMengsi Ruan0Pingbing Zuo1Zilu Zhou2Zhenning Shen3Yi Wang4Xueshang Feng5Chaowei Jiang6Xiaojun Xu7Jiayun Wei8Yanyan Xiong9Ludi Wang10Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macao, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaState Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macao, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaInstitute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, ChinaSolar wind dynamic pressure pulses (DPPs) are small-scale plasma structures with abrupt and large-amplitude plasma dynamic pressure changes on timescales of seconds to several minutes. Overwhelming majority of DPP events (around 79.13%) reside in large-scale solar wind transients, i.e., coronal mass ejections, stream interaction regions, and complex ejecta. In this study, the intermittency, which is a typical feature of solar wind turbulence, is determined and compared during the time intervals in the undisturbed solar wind and in large-scale solar wind transients with clustered DPP events, respectively, as well as in the undisturbed solar wind without DPPs. The probability distribution functions (PDFs) of the fluctuations of proton density increments normalized to the standard deviation at different time lags in the three types of distinct regions are calculated. The PDFs in the undisturbed solar wind without DPPs are near-Gaussian distributions. However, the PDFs in the solar wind with clustered DPPs are obviously non-Gaussian distributions, and the intermittency is much stronger in the large-scale solar wind transients than that in the undisturbed solar wind. The major components of the DPPs are tangential discontinuities (TDs) and rotational discontinuities (RDs), which are suggested to be formed by compressive magnetohydrodynamic (MHD) turbulence. There are far more TD-type DPPs than RD-type DPPs both in the undisturbed solar wind and large-scale solar wind transients. The results imply that the formation of solar wind DPPs could be associated with solar wind turbulence, and much stronger intermittency may be responsible for the high occurrence rate of DPPs in the large-scale solar wind transients.https://www.frontiersin.org/articles/10.3389/fphy.2021.750410/fullsolar wind dynamic pressure pulsediscontinuityturbulenceintermittencydata analysis |
| spellingShingle | Mengsi Ruan Pingbing Zuo Zilu Zhou Zhenning Shen Yi Wang Xueshang Feng Chaowei Jiang Xiaojun Xu Jiayun Wei Yanyan Xiong Ludi Wang The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence Frontiers in Physics solar wind dynamic pressure pulse discontinuity turbulence intermittency data analysis |
| title | The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence |
| title_full | The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence |
| title_fullStr | The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence |
| title_full_unstemmed | The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence |
| title_short | The Relationship Between Solar Wind Dynamic Pressure Pulses and Solar Wind Turbulence |
| title_sort | relationship between solar wind dynamic pressure pulses and solar wind turbulence |
| topic | solar wind dynamic pressure pulse discontinuity turbulence intermittency data analysis |
| url | https://www.frontiersin.org/articles/10.3389/fphy.2021.750410/full |
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