Solar activities associated with ³He-rich solar energetic particle events observed by Solar Orbiter
Abstract
A series of ³He-rich solar energetic particle (SEP) events was observed by Solar Orbiter in May 2021 at a radial distance of 0.95 AU. An isolated active region AR 12824 was likely the ultimate source of these SEP events. The period of the enhanced flux of ³He was also a period of frequent type III bursts in the decametric-hectometric range, confirming their close relationship. As in past studies, we try to find the solar activities possibly responsible for ³He-rich SEP events, using the type III bursts close to the particle injection times estimated from the velocity dispersion. But this exercise is not as straightforward as in many of the past studies since the region produced many more type III bursts and jet-like eruptions than the SEP injections. We may generalize the solar activities for the ³He-rich SEP events in question as coronal jets, but their appearances do not necessarily conform to classic jets that consist of a footpoint and a spire. Conversely, such jets often did not accompany type III bursts. The areas that produced jet-like eruptions changed within the active region from the first to the second set of ³He-rich SEP events, which may be related to the extended coronal mass ejection that launched stealthily.
Additional Information
© 2023 Nitta, Bučík, Mason, Ho, Cohen, Gómez-Herrero, Wang and Balmaceda. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms. We acknowledge the International Space Science Institute (ISSI) for their support of International Team "Origins of ³He-Rich Solar Energetic Particles" (https://www.issibern.ch/teams/origin3henrgpart/). The work of NN was supported by NASA grants 80NSSC18K1126 and 80NSSC20K0287. RB acknowledges support from a NASA grant 80NSSC22K0757. CC was supported by NASA grants 80NSSC18K0223 and 80NSSC21K1512. RG-H acknowledges the financial support of the Spanish MINCIN Project PID2019-104863RBI00/AEI/10.13039/501100011033. Conflict of interest. Author NN was employed by Lockheed Martin Advanced Technology Center. The remaining authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.Attached Files
Published - fspas-10-1148467.pdf
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Additional details
- Eprint ID
- 121120
- Resolver ID
- CaltechAUTHORS:20230420-698969800.7
- NASA
- 80NSSC18K1126
- NASA
- 80NSSC20K0287
- NASA
- 80NSSC22K0757
- NASA
- 80NSSC18K0223
- NASA
- 80NSSC21K1512
- Ministerio de Ciencia e Innovación (MINCIN)
- PID2019-104863RBI00/AEI/10.13039/501100011033
- Created
-
2023-05-03Created from EPrint's datestamp field
- Updated
-
2023-05-03Created from EPrint's last_modified field
- Caltech groups
- Space Radiation Laboratory