How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation
Observations from the second Ulysses fast latitude scan show that the global structure of solar wind near solar maximum is much more complex than at solar minimum. Soon after solar maximum, Ulysses observed a polar coronal hole (high speed) plasma with magnetic polarity of the new solar cycle in the...
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ftcopernicus:oai:publications.copernicus.org:angeo34925 2023-05-15T17:39:53+02:00 How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation Fujiki, K. Kojima, M. Tokumaru, M. Ohmi, T. Yokobe, A. Hayashi, K. McComas, D. J. Elliott, H. A. 2018-09-27 application/pdf https://doi.org/10.5194/angeo-21-1257-2003 https://angeo.copernicus.org/articles/21/1257/2003/ eng eng doi:10.5194/angeo-21-1257-2003 https://angeo.copernicus.org/articles/21/1257/2003/ eISSN: 1432-0576 Text 2018 ftcopernicus https://doi.org/10.5194/angeo-21-1257-2003 2020-07-20T16:27:43Z Observations from the second Ulysses fast latitude scan show that the global structure of solar wind near solar maximum is much more complex than at solar minimum. Soon after solar maximum, Ulysses observed a polar coronal hole (high speed) plasma with magnetic polarity of the new solar cycle in the Northern Hemisphere. We analyze the solar wind structure at and near solar maximum using interplanetary scintillation (IPS) measurements. To do this, we have developed a new tomographic technique, which improves our ability to examine the complex structure of the solar wind at solar maximum. Our IPS results show that in 1999 and 2000 the total area with speed greater than 700 km s -1 is significantly reduced first in the Northern Hemisphere and then in the Southern Hemisphere. For year 2001, we find that the formation of large areas of fast solar wind around the north pole precedes the formation of large polar coronal holes around the southern pole by several months. The IPS observations show a high level agreement to the Ulysses observation, particularly in coronal holes. Key words. Interplanetary physics (solar wind plasma) – Radio science (remote sensing) Text North Pole Copernicus Publications: E-Journals North Pole Annales Geophysicae 21 6 1257 1261 |
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Copernicus Publications: E-Journals |
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English |
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Observations from the second Ulysses fast latitude scan show that the global structure of solar wind near solar maximum is much more complex than at solar minimum. Soon after solar maximum, Ulysses observed a polar coronal hole (high speed) plasma with magnetic polarity of the new solar cycle in the Northern Hemisphere. We analyze the solar wind structure at and near solar maximum using interplanetary scintillation (IPS) measurements. To do this, we have developed a new tomographic technique, which improves our ability to examine the complex structure of the solar wind at solar maximum. Our IPS results show that in 1999 and 2000 the total area with speed greater than 700 km s -1 is significantly reduced first in the Northern Hemisphere and then in the Southern Hemisphere. For year 2001, we find that the formation of large areas of fast solar wind around the north pole precedes the formation of large polar coronal holes around the southern pole by several months. The IPS observations show a high level agreement to the Ulysses observation, particularly in coronal holes. Key words. Interplanetary physics (solar wind plasma) – Radio science (remote sensing) |
format |
Text |
author |
Fujiki, K. Kojima, M. Tokumaru, M. Ohmi, T. Yokobe, A. Hayashi, K. McComas, D. J. Elliott, H. A. |
spellingShingle |
Fujiki, K. Kojima, M. Tokumaru, M. Ohmi, T. Yokobe, A. Hayashi, K. McComas, D. J. Elliott, H. A. How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
author_facet |
Fujiki, K. Kojima, M. Tokumaru, M. Ohmi, T. Yokobe, A. Hayashi, K. McComas, D. J. Elliott, H. A. |
author_sort |
Fujiki, K. |
title |
How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
title_short |
How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
title_full |
How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
title_fullStr |
How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
title_full_unstemmed |
How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation |
title_sort |
how did the solar wind structure change around the solar maximum? from interplanetary scintillation observation |
publishDate |
2018 |
url |
https://doi.org/10.5194/angeo-21-1257-2003 https://angeo.copernicus.org/articles/21/1257/2003/ |
geographic |
North Pole |
geographic_facet |
North Pole |
genre |
North Pole |
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North Pole |
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eISSN: 1432-0576 |
op_relation |
doi:10.5194/angeo-21-1257-2003 https://angeo.copernicus.org/articles/21/1257/2003/ |
op_doi |
https://doi.org/10.5194/angeo-21-1257-2003 |
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Annales Geophysicae |
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21 |
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6 |
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1257 |
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1261 |
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1766140659992887296 |