Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis

Autores
Cheng, I.; Achilleos, N.; Blanco Cano, X.; Bertucci, Cesar; Guio, P.
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The WHAMP (Rönnmark, 1982, https://inis.iaea.org/search/search.aspx?orig_q=RN:14744092)and LEOPARD (Astfalk & Jenko, 2017, https://doi.org/10.1002/2016ja023522) dispersion relation solverswere used to evaluate the growth rate and scale size for mirror mode (MM) and ion cyclotron (IC) instabilitiesunder plasma conditions resembling Saturn's magnetosheath in order to compare observations to predictionsfrom linear kinetic theory. Instabilities and waves are prevalent in planetary magnetosheaths. Understanding theorigin and conditions under which different instabilities grow and dominate can help shed light on the role eachinstability plays in influencing the plasma dynamics of the region. For anisotropic plasmas modeled with bi‐Maxwellian particle distribution, the dispersion, growth rate, and scale size of MM and IC were studied asfunctions of proton temperature anisotropy, proton plasma beta, and oxygen ion abundance. The dispersionsolvers showed that the IC mode dominated over MM under typical conditions in Saturn's magnetosheath, butthat MM could dominate for high enough O+ abundance (>40% ne). These water ion‐rich plasma conditionsare occasionally found in Saturn's magnetosheath (Sergis et al., 2013, https://doi.org/10.1002/jgra.50164). Themaximum linear growth rates (γm/Ωp)for MM ranged from 0.02 to 0.2, larger than expected from observations.The scale size at maximum growth rate ranged from 4 to 12 ρp, smaller than expected from observations. Theseinconsistencies could potentially be attributed to diffusion and non‐linear growth processes.
Fil: Cheng, I.. University College London; Estados Unidos
Fil: Achilleos, N.. University College London; Estados Unidos
Fil: Blanco Cano, X.. Universidad Nacional Autónoma de México; México
Fil: Bertucci, Cesar. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Guio, P.. Arctic University of Norway; Noruega
Materia
SATURN
WAVES
MAGNETOSHEATH
CASSINI
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/264038
Acceder
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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation AnalysisCheng, I.Achilleos, N.Blanco Cano, X.Bertucci, CesarGuio, P.SATURNWAVESMAGNETOSHEATHCASSINIhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The WHAMP (Rönnmark, 1982, https://inis.iaea.org/search/search.aspx?orig_q=RN:14744092)and LEOPARD (Astfalk & Jenko, 2017, https://doi.org/10.1002/2016ja023522) dispersion relation solverswere used to evaluate the growth rate and scale size for mirror mode (MM) and ion cyclotron (IC) instabilitiesunder plasma conditions resembling Saturn's magnetosheath in order to compare observations to predictionsfrom linear kinetic theory. Instabilities and waves are prevalent in planetary magnetosheaths. Understanding theorigin and conditions under which different instabilities grow and dominate can help shed light on the role eachinstability plays in influencing the plasma dynamics of the region. For anisotropic plasmas modeled with bi‐Maxwellian particle distribution, the dispersion, growth rate, and scale size of MM and IC were studied asfunctions of proton temperature anisotropy, proton plasma beta, and oxygen ion abundance. The dispersionsolvers showed that the IC mode dominated over MM under typical conditions in Saturn's magnetosheath, butthat MM could dominate for high enough O+ abundance (>40% ne). These water ion‐rich plasma conditionsare occasionally found in Saturn's magnetosheath (Sergis et al., 2013, https://doi.org/10.1002/jgra.50164). Themaximum linear growth rates (γm/Ωp)for MM ranged from 0.02 to 0.2, larger than expected from observations.The scale size at maximum growth rate ranged from 4 to 12 ρp, smaller than expected from observations. Theseinconsistencies could potentially be attributed to diffusion and non‐linear growth processes.Fil: Cheng, I.. University College London; Estados UnidosFil: Achilleos, N.. University College London; Estados UnidosFil: Blanco Cano, X.. Universidad Nacional Autónoma de México; MéxicoFil: Bertucci, Cesar. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Guio, P.. Arctic University of Norway; NoruegaWiley2024-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/264038Cheng, I.; Achilleos, N.; Blanco Cano, X.; Bertucci, Cesar; Guio, P.; Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis; Wiley; Journal of Geophysical Research: Space Physics; 129; 10; 10-2024; 1-122169-93802169-9402CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2024JA032585info:eu-repo/semantics/altIdentifier/doi/10.1029/2024JA032585info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:42:29Zoai:ri.conicet.gov.ar:11336/264038instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:42:29.494CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
title Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
spellingShingle Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
Cheng, I.
SATURN
WAVES
MAGNETOSHEATH
CASSINI
title_short Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
title_full Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
title_fullStr Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
title_full_unstemmed Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
title_sort Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis
dc.creator.none.fl_str_mv Cheng, I.
Achilleos, N.
Blanco Cano, X.
Bertucci, Cesar
Guio, P.
author Cheng, I.
author_facet Cheng, I.
Achilleos, N.
Blanco Cano, X.
Bertucci, Cesar
Guio, P.
author_role author
author2 Achilleos, N.
Blanco Cano, X.
Bertucci, Cesar
Guio, P.
author2_role author
author
author
author
dc.subject.none.fl_str_mv SATURN
WAVES
MAGNETOSHEATH
CASSINI
topic SATURN
WAVES
MAGNETOSHEATH
CASSINI
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The WHAMP (Rönnmark, 1982, https://inis.iaea.org/search/search.aspx?orig_q=RN:14744092)and LEOPARD (Astfalk & Jenko, 2017, https://doi.org/10.1002/2016ja023522) dispersion relation solverswere used to evaluate the growth rate and scale size for mirror mode (MM) and ion cyclotron (IC) instabilitiesunder plasma conditions resembling Saturn's magnetosheath in order to compare observations to predictionsfrom linear kinetic theory. Instabilities and waves are prevalent in planetary magnetosheaths. Understanding theorigin and conditions under which different instabilities grow and dominate can help shed light on the role eachinstability plays in influencing the plasma dynamics of the region. For anisotropic plasmas modeled with bi‐Maxwellian particle distribution, the dispersion, growth rate, and scale size of MM and IC were studied asfunctions of proton temperature anisotropy, proton plasma beta, and oxygen ion abundance. The dispersionsolvers showed that the IC mode dominated over MM under typical conditions in Saturn's magnetosheath, butthat MM could dominate for high enough O+ abundance (>40% ne). These water ion‐rich plasma conditionsare occasionally found in Saturn's magnetosheath (Sergis et al., 2013, https://doi.org/10.1002/jgra.50164). Themaximum linear growth rates (γm/Ωp)for MM ranged from 0.02 to 0.2, larger than expected from observations.The scale size at maximum growth rate ranged from 4 to 12 ρp, smaller than expected from observations. Theseinconsistencies could potentially be attributed to diffusion and non‐linear growth processes.
Fil: Cheng, I.. University College London; Estados Unidos
Fil: Achilleos, N.. University College London; Estados Unidos
Fil: Blanco Cano, X.. Universidad Nacional Autónoma de México; México
Fil: Bertucci, Cesar. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Guio, P.. Arctic University of Norway; Noruega
description The WHAMP (Rönnmark, 1982, https://inis.iaea.org/search/search.aspx?orig_q=RN:14744092)and LEOPARD (Astfalk & Jenko, 2017, https://doi.org/10.1002/2016ja023522) dispersion relation solverswere used to evaluate the growth rate and scale size for mirror mode (MM) and ion cyclotron (IC) instabilitiesunder plasma conditions resembling Saturn's magnetosheath in order to compare observations to predictionsfrom linear kinetic theory. Instabilities and waves are prevalent in planetary magnetosheaths. Understanding theorigin and conditions under which different instabilities grow and dominate can help shed light on the role eachinstability plays in influencing the plasma dynamics of the region. For anisotropic plasmas modeled with bi‐Maxwellian particle distribution, the dispersion, growth rate, and scale size of MM and IC were studied asfunctions of proton temperature anisotropy, proton plasma beta, and oxygen ion abundance. The dispersionsolvers showed that the IC mode dominated over MM under typical conditions in Saturn's magnetosheath, butthat MM could dominate for high enough O+ abundance (>40% ne). These water ion‐rich plasma conditionsare occasionally found in Saturn's magnetosheath (Sergis et al., 2013, https://doi.org/10.1002/jgra.50164). Themaximum linear growth rates (γm/Ωp)for MM ranged from 0.02 to 0.2, larger than expected from observations.The scale size at maximum growth rate ranged from 4 to 12 ρp, smaller than expected from observations. Theseinconsistencies could potentially be attributed to diffusion and non‐linear growth processes.
publishDate 2024
dc.date.none.fl_str_mv 2024-10
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/264038
Cheng, I.; Achilleos, N.; Blanco Cano, X.; Bertucci, Cesar; Guio, P.; Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis; Wiley; Journal of Geophysical Research: Space Physics; 129; 10; 10-2024; 1-12
2169-9380
2169-9402
CONICET Digital
CONICET
url http://hdl.handle.net/11336/264038
identifier_str_mv Cheng, I.; Achilleos, N.; Blanco Cano, X.; Bertucci, Cesar; Guio, P.; Waves and Instabilities in Saturn's Magnetosheath: 2. Dispersion Relation Analysis; Wiley; Journal of Geophysical Research: Space Physics; 129; 10; 10-2024; 1-12
2169-9380
2169-9402
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2024JA032585
info:eu-repo/semantics/altIdentifier/doi/10.1029/2024JA032585
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley
publisher.none.fl_str_mv Wiley
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.22299

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