Saved in:
| Main Authors: | , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2401.10863 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866914646244458496 |
|---|---|
| author | Bisoi, Susanta Kumar Rout, Diptiranjan Janardhan, P. Fujiki, K. Chakrabarty, Dibyendu Sahu, Karan |
| author_facet | Bisoi, Susanta Kumar Rout, Diptiranjan Janardhan, P. Fujiki, K. Chakrabarty, Dibyendu Sahu, Karan |
| contents | We present a study of three highly non-radial solar wind events when the azimuthal solar wind flow angle exceeds > 6 degrees for one day or more. None of the events are associated with coronal mass ejections and co-rotating interaction regions observed at 1 AU. For all events, the solar wind outflows at 1 AU have low solar wind velocity and solar wind density. Based on the significant increase in the Oxygen charge state ratio of O7+/O6+ at 1 AU for all of the events, we have traced them back to the Sun and found that their source regions originated in an active region and coronal hole (AR-CH) pairs mainly located at the central meridian. Further, examining the dynamical evolutions in their source regions using both the Extreme ultra-violet Imaging Telescope and Michelson Doppler Imager, it is found that the changes taking place in AR-CH boundaries eventually disturbed the stable CH configurations, resulting in a reduction of the CH area and finally its disappearance, leaving only with the AR. Our study provides a possible explanation to discuss the origin of the prolonged and highly non-radial solar wind flows. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_10863 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Prolonged and Extremely Non-radial Solar Wind Flows Bisoi, Susanta Kumar Rout, Diptiranjan Janardhan, P. Fujiki, K. Chakrabarty, Dibyendu Sahu, Karan Solar and Stellar Astrophysics Space Physics We present a study of three highly non-radial solar wind events when the azimuthal solar wind flow angle exceeds > 6 degrees for one day or more. None of the events are associated with coronal mass ejections and co-rotating interaction regions observed at 1 AU. For all events, the solar wind outflows at 1 AU have low solar wind velocity and solar wind density. Based on the significant increase in the Oxygen charge state ratio of O7+/O6+ at 1 AU for all of the events, we have traced them back to the Sun and found that their source regions originated in an active region and coronal hole (AR-CH) pairs mainly located at the central meridian. Further, examining the dynamical evolutions in their source regions using both the Extreme ultra-violet Imaging Telescope and Michelson Doppler Imager, it is found that the changes taking place in AR-CH boundaries eventually disturbed the stable CH configurations, resulting in a reduction of the CH area and finally its disappearance, leaving only with the AR. Our study provides a possible explanation to discuss the origin of the prolonged and highly non-radial solar wind flows. |
| title | Prolonged and Extremely Non-radial Solar Wind Flows |
| topic | Solar and Stellar Astrophysics Space Physics |
| url | https://arxiv.org/abs/2401.10863 |