How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation
International audience 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...
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ftccsdartic:oai:HAL:hal-00317078v1 2023-11-12T04:23:03+01:00 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. Solar-Terrestrial Environment Laboratory Nagoya (STEL) Nagoya University SGI Japan Ltd. Southwest Research Institute San Antonio (SwRI) 2003 https://hal.science/hal-00317078 https://hal.science/hal-00317078/document https://hal.science/hal-00317078/file/angeo-21-1257-2003.pdf en eng HAL CCSD European Geosciences Union hal-00317078 https://hal.science/hal-00317078 https://hal.science/hal-00317078/document https://hal.science/hal-00317078/file/angeo-21-1257-2003.pdf info:eu-repo/semantics/OpenAccess ISSN: 0992-7689 EISSN: 1432-0576 Annales Geophysicae https://hal.science/hal-00317078 Annales Geophysicae, 2003, 21 (6), pp.1257-1261 [SDU.OCEAN]Sciences of the Universe [physics]/Ocean Atmosphere [SDU.STU]Sciences of the Universe [physics]/Earth Sciences info:eu-repo/semantics/article Journal articles 2003 ftccsdartic 2023-10-21T23:07:48Z International audience 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. Article in Journal/Newspaper North Pole Archive ouverte HAL (Hyper Article en Ligne, CCSD - Centre pour la Communication Scientifique Directe) North Pole |
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Archive ouverte HAL (Hyper Article en Ligne, CCSD - Centre pour la Communication Scientifique Directe) |
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ftccsdartic |
language |
English |
topic |
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean Atmosphere [SDU.STU]Sciences of the Universe [physics]/Earth Sciences |
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[SDU.OCEAN]Sciences of the Universe [physics]/Ocean Atmosphere [SDU.STU]Sciences of the Universe [physics]/Earth Sciences 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 |
topic_facet |
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean Atmosphere [SDU.STU]Sciences of the Universe [physics]/Earth Sciences |
description |
International audience 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. |
author2 |
Solar-Terrestrial Environment Laboratory Nagoya (STEL) Nagoya University SGI Japan Ltd. Southwest Research Institute San Antonio (SwRI) |
format |
Article in Journal/Newspaper |
author |
Fujiki, K. Kojima, M. Tokumaru, M. Ohmi, T. Yokobe, A. Hayashi, K. Mccomas, D. J. Elliott, H. A. |
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 |
publisher |
HAL CCSD |
publishDate |
2003 |
url |
https://hal.science/hal-00317078 https://hal.science/hal-00317078/document https://hal.science/hal-00317078/file/angeo-21-1257-2003.pdf |
geographic |
North Pole |
geographic_facet |
North Pole |
genre |
North Pole |
genre_facet |
North Pole |
op_source |
ISSN: 0992-7689 EISSN: 1432-0576 Annales Geophysicae https://hal.science/hal-00317078 Annales Geophysicae, 2003, 21 (6), pp.1257-1261 |
op_relation |
hal-00317078 https://hal.science/hal-00317078 https://hal.science/hal-00317078/document https://hal.science/hal-00317078/file/angeo-21-1257-2003.pdf |
op_rights |
info:eu-repo/semantics/OpenAccess |
_version_ |
1782337938275696640 |