Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams
Energetic proton events associated with a stream interaction region (SIR) were observed by two Solar-Terrestrial Relations Observatory (STEREO) and WIND spacecraft from 2007 September 19 to September 25. Different from the measurements of STEREO-A and WIND, the observational data of STEREO-B show ad...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad96ae |
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| author | Xinyi Tao Fang Shen Xi Luo |
| author_facet | Xinyi Tao Fang Shen Xi Luo |
| author_sort | Xinyi Tao |
| collection | DOAJ |
| description | Energetic proton events associated with a stream interaction region (SIR) were observed by two Solar-Terrestrial Relations Observatory (STEREO) and WIND spacecraft from 2007 September 19 to September 25. Different from the measurements of STEREO-A and WIND, the observational data of STEREO-B show additional particle intensity increases when the spacecraft is immersed into the compound stream region with poor compression signatures after the passage of the SIR. In order to investigate this particular event, we simulated proton transport with a solar wind pattern obtained from the two-dimensional analytical model driven by plasma and magnetic field data of the spacecraft. We find that the additional energetic proton event is not an autonomous event created by the compound streams and is closely associated with the accelerated particles in the preceding SIR structure. We highlight the variation in particle distribution as a function of radial distance within the SIR. The magnetic field configuration in the compound stream region observed by STEREO-B provides a more direct connection to the source particle region, which presents a view to explain the differences between the energetic proton observations of the three spacecraft. |
| format | Article |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-56733d69c7cd4a1a941f21ae2fd975f62025-01-07T06:40:37ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01978214310.3847/1538-4357/ad96aeModeling Energetic Proton Transport from a Stream Interaction Region to Compound StreamsXinyi Tao0Fang Shen1https://orcid.org/0000-0002-4935-6679Xi Luo2https://orcid.org/0000-0002-4508-6042Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China ; fshen@spaceweather.ac.cn; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China ; fshen@spaceweather.ac.cn; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaShandong Institute of Advanced Technology , Jinan 250100, People’s Republic of ChinaEnergetic proton events associated with a stream interaction region (SIR) were observed by two Solar-Terrestrial Relations Observatory (STEREO) and WIND spacecraft from 2007 September 19 to September 25. Different from the measurements of STEREO-A and WIND, the observational data of STEREO-B show additional particle intensity increases when the spacecraft is immersed into the compound stream region with poor compression signatures after the passage of the SIR. In order to investigate this particular event, we simulated proton transport with a solar wind pattern obtained from the two-dimensional analytical model driven by plasma and magnetic field data of the spacecraft. We find that the additional energetic proton event is not an autonomous event created by the compound streams and is closely associated with the accelerated particles in the preceding SIR structure. We highlight the variation in particle distribution as a function of radial distance within the SIR. The magnetic field configuration in the compound stream region observed by STEREO-B provides a more direct connection to the source particle region, which presents a view to explain the differences between the energetic proton observations of the three spacecraft.https://doi.org/10.3847/1538-4357/ad96aeCorotating streamsInterplanetary particle accelerationMagnetic fieldsSolar wind |
| spellingShingle | Xinyi Tao Fang Shen Xi Luo Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams The Astrophysical Journal Corotating streams Interplanetary particle acceleration Magnetic fields Solar wind |
| title | Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams |
| title_full | Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams |
| title_fullStr | Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams |
| title_full_unstemmed | Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams |
| title_short | Modeling Energetic Proton Transport from a Stream Interaction Region to Compound Streams |
| title_sort | modeling energetic proton transport from a stream interaction region to compound streams |
| topic | Corotating streams Interplanetary particle acceleration Magnetic fields Solar wind |
| url | https://doi.org/10.3847/1538-4357/ad96ae |
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