Solar Wind Structures from the Gaussianity of Magnetic Magnitude
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arXiv
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| Auteurs principaux: | , , , , , , , , , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866929628200828928 |
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| author | Huang, Zesen Shi, Chen Velli, Marco Sioulas, Nikos Panasenco, Olga Bowen, Trevor Matteini, Lorenzo Xia, Mingtao Shi, Xiaofei Huang, Sheng Huang, Jia Casillas, Lizet |
| author_facet | Huang, Zesen Shi, Chen Velli, Marco Sioulas, Nikos Panasenco, Olga Bowen, Trevor Matteini, Lorenzo Xia, Mingtao Shi, Xiaofei Huang, Sheng Huang, Jia Casillas, Lizet |
| contents | One of the primary science objectives of Parker Solar Probe (PSP) is to determine the structures and dynamics of the plasma and magnetic fields at the sources of the solar wind. However, establishing the connection between {\it in situ} measurements and structures and dynamics in the solar atmosphere is challenging: most of the magnetic footpoint mapping techniques have significant uncertainties in the source localization of a plasma parcel observed {\it in situ}, and the PSP plasma measurements suffer from a limited field of view. Therefore it is of interest to investigate whether {\it in situ} measurements can be used on their own to identify streams originating from the same structures in the corona more finely than the well known fast wind-coronal hole, slow wind-elsewhere distinction. Here we develop a novel time series visualization method \textcolor{red}{(time-frequency representation or TFR)} named Gaussianity Scalogram. Utilizing this method, by analyzing the magnetic magnitude data from both PSP and Ulysses, we successfully identify {\it in situ} structures that are possible remnants of solar atmospheric and magnetic structures spanning more than seven orders of magnitude, from years to seconds, including polar and mid-latitude coronal holes, as well as structures compatible with super-granulation , ``jetlets'' and ``picoflares''. \textcolor{red}{Furthermore, computer simulations of Alfvénic turbulence successfully reproduce the Gaussianization of the magnetic magnitude for locally homogeneous structures.} Building upon these discoveries, the Gaussianity Scalogram can help future studies to reveal the fractal-like fine structures in the solar wind time series from both PSP and decades-old data archive. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2312_08669 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Solar Wind Structures from the Gaussianity of Magnetic Magnitude Huang, Zesen Shi, Chen Velli, Marco Sioulas, Nikos Panasenco, Olga Bowen, Trevor Matteini, Lorenzo Xia, Mingtao Shi, Xiaofei Huang, Sheng Huang, Jia Casillas, Lizet Space Physics Solar and Stellar Astrophysics One of the primary science objectives of Parker Solar Probe (PSP) is to determine the structures and dynamics of the plasma and magnetic fields at the sources of the solar wind. However, establishing the connection between {\it in situ} measurements and structures and dynamics in the solar atmosphere is challenging: most of the magnetic footpoint mapping techniques have significant uncertainties in the source localization of a plasma parcel observed {\it in situ}, and the PSP plasma measurements suffer from a limited field of view. Therefore it is of interest to investigate whether {\it in situ} measurements can be used on their own to identify streams originating from the same structures in the corona more finely than the well known fast wind-coronal hole, slow wind-elsewhere distinction. Here we develop a novel time series visualization method \textcolor{red}{(time-frequency representation or TFR)} named Gaussianity Scalogram. Utilizing this method, by analyzing the magnetic magnitude data from both PSP and Ulysses, we successfully identify {\it in situ} structures that are possible remnants of solar atmospheric and magnetic structures spanning more than seven orders of magnitude, from years to seconds, including polar and mid-latitude coronal holes, as well as structures compatible with super-granulation , ``jetlets'' and ``picoflares''. \textcolor{red}{Furthermore, computer simulations of Alfvénic turbulence successfully reproduce the Gaussianization of the magnetic magnitude for locally homogeneous structures.} Building upon these discoveries, the Gaussianity Scalogram can help future studies to reveal the fractal-like fine structures in the solar wind time series from both PSP and decades-old data archive. |
| title | Solar Wind Structures from the Gaussianity of Magnetic Magnitude |
| topic | Space Physics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2312.08669 |