The Evolution of Ion Charge States in Coronal Mass Ejections
We model the observed charge states of the elements C, O, Mg, Si, and Fe in the ejecta of coronal mass ejections (CMEs). We concentrate on “halo” CMEs observed in situ by the Advanced Composition Explorer/Solar Wind Ion Composition Spectrometer to measure ion charge states, and also remotely by the...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acebc2 |
| _version_ | 1827854392187944960 |
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| author | J. Martin Laming Elena Provornikova Yuan-Kuen Ko |
| author_facet | J. Martin Laming Elena Provornikova Yuan-Kuen Ko |
| author_sort | J. Martin Laming |
| collection | DOAJ |
| description | We model the observed charge states of the elements C, O, Mg, Si, and Fe in the ejecta of coronal mass ejections (CMEs). We concentrate on “halo” CMEs observed in situ by the Advanced Composition Explorer/Solar Wind Ion Composition Spectrometer to measure ion charge states, and also remotely by the Solar Terrestrial Relations Observatory when in near quadrature with the Earth, so that the CME expansion can be accurately specified. Within this observed expansion, we integrate equations for the CME ejecta ionization balance, including electron heating parameterized as a fraction of the kinetic and gravitational energy gain of the CME. We also include the effects of non-Maxwellian electron distributions, characterized as a κ function. Focusing first on the 2010 April 3 CME, we find a somewhat better match to the observed charge states with κ close to the theoretical minimum value of κ = 3/2, implying a hard spectrum of nonthermal electrons. Similar but more significant results come from the 2011 February 15 event, although it is quite different in terms of its evolution. We discuss the implications of these values, and of the heating required, in terms of the magnetic reconnection Lundquist number and anomalous resistivity associated with CME evolution close to the Sun. |
| first_indexed | 2024-03-12T11:22:06Z |
| format | Article |
| id | doaj.art-9a26b9ec41be4cb08e6428b2782d3759 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T11:22:06Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-9a26b9ec41be4cb08e6428b2782d37592023-09-01T17:19:54ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01954214510.3847/1538-4357/acebc2The Evolution of Ion Charge States in Coronal Mass EjectionsJ. Martin Laming0https://orcid.org/0000-0002-3362-7040Elena Provornikova1https://orcid.org/0000-0001-8875-7478Yuan-Kuen Ko2https://orcid.org/0000-0002-8747-4772Space Science Division, Code 7684, Naval Research Laboratory , Washington DC 20375, USA ; j.laming@nrl.navy.milThe Johns Hopkins University Applied Physics Laboratory , Laurel, MD 20723, USASpace Science Division, Code 7684, Naval Research Laboratory , Washington DC 20375, USA ; j.laming@nrl.navy.milWe model the observed charge states of the elements C, O, Mg, Si, and Fe in the ejecta of coronal mass ejections (CMEs). We concentrate on “halo” CMEs observed in situ by the Advanced Composition Explorer/Solar Wind Ion Composition Spectrometer to measure ion charge states, and also remotely by the Solar Terrestrial Relations Observatory when in near quadrature with the Earth, so that the CME expansion can be accurately specified. Within this observed expansion, we integrate equations for the CME ejecta ionization balance, including electron heating parameterized as a fraction of the kinetic and gravitational energy gain of the CME. We also include the effects of non-Maxwellian electron distributions, characterized as a κ function. Focusing first on the 2010 April 3 CME, we find a somewhat better match to the observed charge states with κ close to the theoretical minimum value of κ = 3/2, implying a hard spectrum of nonthermal electrons. Similar but more significant results come from the 2011 February 15 event, although it is quite different in terms of its evolution. We discuss the implications of these values, and of the heating required, in terms of the magnetic reconnection Lundquist number and anomalous resistivity associated with CME evolution close to the Sun.https://doi.org/10.3847/1538-4357/acebc2Solar magnetic reconnectionSolar coronal mass ejectionsEjecta |
| spellingShingle | J. Martin Laming Elena Provornikova Yuan-Kuen Ko The Evolution of Ion Charge States in Coronal Mass Ejections The Astrophysical Journal Solar magnetic reconnection Solar coronal mass ejections Ejecta |
| title | The Evolution of Ion Charge States in Coronal Mass Ejections |
| title_full | The Evolution of Ion Charge States in Coronal Mass Ejections |
| title_fullStr | The Evolution of Ion Charge States in Coronal Mass Ejections |
| title_full_unstemmed | The Evolution of Ion Charge States in Coronal Mass Ejections |
| title_short | The Evolution of Ion Charge States in Coronal Mass Ejections |
| title_sort | evolution of ion charge states in coronal mass ejections |
| topic | Solar magnetic reconnection Solar coronal mass ejections Ejecta |
| url | https://doi.org/10.3847/1538-4357/acebc2 |
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