Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere
Models currently fail to reproduce observations of the coldest regions in the Sun’s atmosphere, though recent work suggests the thermal Farley–Buneman instability (TFBI) may play a critical role. This meter-scale, electrostatic, multifluid plasma instability causes turbulence and heating in the cold...
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| Language: | English |
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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/adcd70 |
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| author | Samuel Evans Meers Oppenheim Juan Martínez-Sykora Yakov Dimant |
| author_facet | Samuel Evans Meers Oppenheim Juan Martínez-Sykora Yakov Dimant |
| author_sort | Samuel Evans |
| collection | DOAJ |
| description | Models currently fail to reproduce observations of the coldest regions in the Sun’s atmosphere, though recent work suggests the thermal Farley–Buneman instability (TFBI) may play a critical role. This meter-scale, electrostatic, multifluid plasma instability causes turbulence and heating in the coldest regions of the solar chromosphere. This paper describes how TFBI turbulence and heating varies across multifluid 2D, kinetic 2D, and kinetic 3D simulations. It also presents the first 3D simulations of the TFBI. We find that multifluid and kinetic 2D simulations produce similar results overall, despite using vastly different approaches. Additionally, our kinetic 3D simulations produce a similar or somewhat larger amount of heating compared to 2D, as contributions from the parallel electric field account for only (13 ± 2.5)% of the total turbulent heating in 3D. |
| format | Article |
| id | doaj-art-151a86457a654d5282cbd1ba3d4d1d1c |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-151a86457a654d5282cbd1ba3d4d1d1c2025-08-20T03:07:37ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198612310.3847/1538-4357/adcd70Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar ChromosphereSamuel Evans0https://orcid.org/0000-0002-1127-7350Meers Oppenheim1https://orcid.org/0000-0002-8581-6177Juan Martínez-Sykora2https://orcid.org/0000-0002-0333-5717Yakov Dimant3https://orcid.org/0000-0002-3807-5820Boston University Center for Space Physics , 725 Commonwealth Ave, Boston, MA 02215, USA ; sevans7@bu.eduBoston University Center for Space Physics , 725 Commonwealth Ave, Boston, MA 02215, USA ; sevans7@bu.eduLockheed Martin Solar & Astrophysics Laboratory , 3251 Hanover St, Palo Alto, CA 94304, USA; Bay Area Environmental Research Institute , NASA Research Park, Moffett Field, CA 94035, USA; Rosseland Centre for Solar Physics, University of Oslo , P.O. Box 1029 Blindern, N-0315 Oslo, Norway; Institute of Theoretical Astrophysics, University of Oslo , P.O. Box 1029 Blindern, N-0315 Oslo, NorwayBoston University Center for Space Physics , 725 Commonwealth Ave, Boston, MA 02215, USA ; sevans7@bu.eduModels currently fail to reproduce observations of the coldest regions in the Sun’s atmosphere, though recent work suggests the thermal Farley–Buneman instability (TFBI) may play a critical role. This meter-scale, electrostatic, multifluid plasma instability causes turbulence and heating in the coldest regions of the solar chromosphere. This paper describes how TFBI turbulence and heating varies across multifluid 2D, kinetic 2D, and kinetic 3D simulations. It also presents the first 3D simulations of the TFBI. We find that multifluid and kinetic 2D simulations produce similar results overall, despite using vastly different approaches. Additionally, our kinetic 3D simulations produce a similar or somewhat larger amount of heating compared to 2D, as contributions from the parallel electric field account for only (13 ± 2.5)% of the total turbulent heating in 3D.https://doi.org/10.3847/1538-4357/adcd70Solar chromosphereSolar chromospheric heatingPlasma physicsAstronomical simulations |
| spellingShingle | Samuel Evans Meers Oppenheim Juan Martínez-Sykora Yakov Dimant Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere The Astrophysical Journal Solar chromosphere Solar chromospheric heating Plasma physics Astronomical simulations |
| title | Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere |
| title_full | Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere |
| title_fullStr | Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere |
| title_full_unstemmed | Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere |
| title_short | Multifluid and Kinetic 2D and 3D Simulations of Thermal Farley–Buneman Instability Turbulence in the Solar Chromosphere |
| title_sort | multifluid and kinetic 2d and 3d simulations of thermal farley buneman instability turbulence in the solar chromosphere |
| topic | Solar chromosphere Solar chromospheric heating Plasma physics Astronomical simulations |
| url | https://doi.org/10.3847/1538-4357/adcd70 |
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