Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks
Shocks associated with interplanetary coronal mass ejections are known to energize charged particles and give rise to solar energetic particles. Many of these energetic particles move ahead of the shock to create a foreshock region. The foreshock region primarily consists of solar wind plasma, exhib...
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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/add3f0 |
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| author | Shanwlee Sow Mondal Aveek Sarkar Sofiane Bourouaine |
| author_facet | Shanwlee Sow Mondal Aveek Sarkar Sofiane Bourouaine |
| author_sort | Shanwlee Sow Mondal |
| collection | DOAJ |
| description | Shocks associated with interplanetary coronal mass ejections are known to energize charged particles and give rise to solar energetic particles. Many of these energetic particles move ahead of the shock to create a foreshock region. The foreshock region primarily consists of solar wind plasma, exhibiting turbulent velocity and magnetic fields. Such turbulent behavior results from inherent solar wind turbulence modified by energetic particles. We analyze magnetic field data from six such ICME shocks observed by the Wind spacecraft. The analysis of the shock upstream shows that the magnetic power spectral density (PSD) maintains a power-law slope of −5/3. We also identify clear intermittent peaks in the PSD. After characterizing these peaks, we investigate various possibilities for their generation. Our analysis indicates that these peaks in the PSD are due to the resonant interaction of Alfvén waves with the bulk solar wind protons and protons with energy up to 10 keV. However, evidence of Alfvén wave interaction with highly energetic protons is not evident in our analysis, and we anticipate that such evidence is obscured by the prevailing solar wind turbulence in the shock upstream. |
| format | Article |
| id | doaj-art-0cc36e035cfe4aee965f01be38f19cf1 |
| institution | Matheson Library |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-0cc36e035cfe4aee965f01be38f19cf12025-06-28T16:34:25ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198715510.3847/1538-4357/add3f0Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection ShocksShanwlee Sow Mondal0https://orcid.org/0000-0003-4225-8520Aveek Sarkar1https://orcid.org/0000-0002-4781-5798Sofiane Bourouaine2https://orcid.org/0000-0002-2358-6628Astronomy and Astrophysics Division , Physical Research Laboratory, Ahmedabad 380009, India; The Catholic University of America , 620 Michigan Ave., N.E. Washington, DC 20064, USA; NASA Goddard Space Flight Center , 8800 Greenbelt Rd., Greenbelt, MD 20771, USAAstronomy and Astrophysics Division , Physical Research Laboratory, Ahmedabad 380009, IndiaDepartment of Aerospace, Physics and Space Sciences, Florida Institute of Technology , Melbourne, FL 32901, USAShocks associated with interplanetary coronal mass ejections are known to energize charged particles and give rise to solar energetic particles. Many of these energetic particles move ahead of the shock to create a foreshock region. The foreshock region primarily consists of solar wind plasma, exhibiting turbulent velocity and magnetic fields. Such turbulent behavior results from inherent solar wind turbulence modified by energetic particles. We analyze magnetic field data from six such ICME shocks observed by the Wind spacecraft. The analysis of the shock upstream shows that the magnetic power spectral density (PSD) maintains a power-law slope of −5/3. We also identify clear intermittent peaks in the PSD. After characterizing these peaks, we investigate various possibilities for their generation. Our analysis indicates that these peaks in the PSD are due to the resonant interaction of Alfvén waves with the bulk solar wind protons and protons with energy up to 10 keV. However, evidence of Alfvén wave interaction with highly energetic protons is not evident in our analysis, and we anticipate that such evidence is obscured by the prevailing solar wind turbulence in the shock upstream.https://doi.org/10.3847/1538-4357/add3f0Solar coronal mass ejection shocksSolar energetic particlesHeliosphereAlfvén waves |
| spellingShingle | Shanwlee Sow Mondal Aveek Sarkar Sofiane Bourouaine Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks The Astrophysical Journal Solar coronal mass ejection shocks Solar energetic particles Heliosphere Alfvén waves |
| title | Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks |
| title_full | Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks |
| title_fullStr | Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks |
| title_full_unstemmed | Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks |
| title_short | Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks |
| title_sort | wave particle interaction in the upstream of interplanetary coronal mass ejection shocks |
| topic | Solar coronal mass ejection shocks Solar energetic particles Heliosphere Alfvén waves |
| url | https://doi.org/10.3847/1538-4357/add3f0 |
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