Prolonged and Extremely Non-radial Solar Wind Flows

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 outf...

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Bibliographic Details
Published inarXiv.org
Main Authors Bisoi, Susanta Kumar, Rout, Diptiranjan, Janardhan, P, Fujiki, K, Chakrabarty, Dibyendu, Sahu, Karan
Format Paper
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 19.01.2024
Subjects
Coronal holes
Coronal mass ejection
Solar wind
Solar wind velocity
Wind speed
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Summary: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.
ISSN:2331-8422