The variability of Titan's magnetic environment

Autores
Bertucci, Cesar; Sinclair, B.; Achilleos, N.; Hunt, P.; Dougherty, M. K.; Arridge, C. S.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
With a mean orbital radius of 20.2 Saturnian radii (1 Saturn radius RS=60,330 km), Titan is usually located within the kronian magnetosphere. 3.5 years of Cassini magnetometer observations in the vicinity of Titan´s orbit reveal that the moon´s magnetic environment is strongly affected by the presence of Saturn´s magnetodisk. As a result of the disk´s solar-wind-induced asymmetry, Titan is exposed to quasi-dipolar fields in the noon sector, and planetward, swept-back fields in the dawn, dusk and midnight sectors. These magnetic properties indicate that the moon is, on average, south of the central current sheet and immersed in Saturn´s rotating magnetospheric plasma for all local times (SLT). At a given SLT, Titan´s distance from the central current sheet associated with the magnetodisk depends on the solar wind pressure and on the phase of the Saturn´s kilometric radiation (SKR). The influence of the solar wind is present at all SLT (although dominant in the noon sector), whereas the SKR modulation seems to affect the magnetic field to first-order at least in the dawn sector. Near dawn local times, Titan tends to be farther from the disk at SKR longitudes around ˜140° and closer to it for longitudes around ˜320°. Depending on these factors, Titan is exposed to either: (i) a ‘magnetodisk lobe’ regime where the plasma beta is low and fields are radially ‘stretched’ and usually stronger or (ii) a ‘current sheet’ regime—characterized by quasi-dipolar, relatively weak fields and a high-beta plasma.
Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes 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. Imperial College London; Reino Unido
Fil: Sinclair, B.. Imperial College London; Reino Unido
Fil: Achilleos, N.. University College London; Estados Unidos
Fil: Hunt, P.. Imperial College London; Reino Unido
Fil: Dougherty, M. K.. Imperial College London; Reino Unido
Fil: Arridge, C. S.. University College London; Estados Unidos
Materia
Planetary Magnetospheres
Magnetodisk
Titan
Plasma Interactions with Unmagnetized Bodies
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/20687
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The variability of Titan's magnetic environmentBertucci, CesarSinclair, B.Achilleos, N.Hunt, P.Dougherty, M. K.Arridge, C. S.Planetary MagnetospheresMagnetodiskTitanPlasma Interactions with Unmagnetized Bodieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1With a mean orbital radius of 20.2 Saturnian radii (1 Saturn radius RS=60,330 km), Titan is usually located within the kronian magnetosphere. 3.5 years of Cassini magnetometer observations in the vicinity of Titan´s orbit reveal that the moon´s magnetic environment is strongly affected by the presence of Saturn´s magnetodisk. As a result of the disk´s solar-wind-induced asymmetry, Titan is exposed to quasi-dipolar fields in the noon sector, and planetward, swept-back fields in the dawn, dusk and midnight sectors. These magnetic properties indicate that the moon is, on average, south of the central current sheet and immersed in Saturn´s rotating magnetospheric plasma for all local times (SLT). At a given SLT, Titan´s distance from the central current sheet associated with the magnetodisk depends on the solar wind pressure and on the phase of the Saturn´s kilometric radiation (SKR). The influence of the solar wind is present at all SLT (although dominant in the noon sector), whereas the SKR modulation seems to affect the magnetic field to first-order at least in the dawn sector. Near dawn local times, Titan tends to be farther from the disk at SKR longitudes around ˜140° and closer to it for longitudes around ˜320°. Depending on these factors, Titan is exposed to either: (i) a ‘magnetodisk lobe’ regime where the plasma beta is low and fields are radially ‘stretched’ and usually stronger or (ii) a ‘current sheet’ regime—characterized by quasi-dipolar, relatively weak fields and a high-beta plasma.Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes 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. Imperial College London; Reino UnidoFil: Sinclair, B.. Imperial College London; Reino UnidoFil: Achilleos, N.. University College London; Estados UnidosFil: Hunt, P.. Imperial College London; Reino UnidoFil: Dougherty, M. K.. Imperial College London; Reino UnidoFil: Arridge, C. S.. University College London; Estados UnidosElsevier2009-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20687Bertucci, Cesar; Sinclair, B.; Achilleos, N.; Hunt, P.; Dougherty, M. K.; et al.; The variability of Titan's magnetic environment; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1813-18200032-0633CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2009.02.009info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063309000543info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:30:27Zoai:ri.conicet.gov.ar:11336/20687instacron: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 14:30:27.3CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The variability of Titan's magnetic environment
title The variability of Titan's magnetic environment
spellingShingle The variability of Titan's magnetic environment
Bertucci, Cesar
Planetary Magnetospheres
Magnetodisk
Titan
Plasma Interactions with Unmagnetized Bodies
title_short The variability of Titan's magnetic environment
title_full The variability of Titan's magnetic environment
title_fullStr The variability of Titan's magnetic environment
title_full_unstemmed The variability of Titan's magnetic environment
title_sort The variability of Titan's magnetic environment
dc.creator.none.fl_str_mv Bertucci, Cesar
Sinclair, B.
Achilleos, N.
Hunt, P.
Dougherty, M. K.
Arridge, C. S.
author Bertucci, Cesar
author_facet Bertucci, Cesar
Sinclair, B.
Achilleos, N.
Hunt, P.
Dougherty, M. K.
Arridge, C. S.
author_role author
author2 Sinclair, B.
Achilleos, N.
Hunt, P.
Dougherty, M. K.
Arridge, C. S.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Planetary Magnetospheres
Magnetodisk
Titan
Plasma Interactions with Unmagnetized Bodies
topic Planetary Magnetospheres
Magnetodisk
Titan
Plasma Interactions with Unmagnetized Bodies
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv With a mean orbital radius of 20.2 Saturnian radii (1 Saturn radius RS=60,330 km), Titan is usually located within the kronian magnetosphere. 3.5 years of Cassini magnetometer observations in the vicinity of Titan´s orbit reveal that the moon´s magnetic environment is strongly affected by the presence of Saturn´s magnetodisk. As a result of the disk´s solar-wind-induced asymmetry, Titan is exposed to quasi-dipolar fields in the noon sector, and planetward, swept-back fields in the dawn, dusk and midnight sectors. These magnetic properties indicate that the moon is, on average, south of the central current sheet and immersed in Saturn´s rotating magnetospheric plasma for all local times (SLT). At a given SLT, Titan´s distance from the central current sheet associated with the magnetodisk depends on the solar wind pressure and on the phase of the Saturn´s kilometric radiation (SKR). The influence of the solar wind is present at all SLT (although dominant in the noon sector), whereas the SKR modulation seems to affect the magnetic field to first-order at least in the dawn sector. Near dawn local times, Titan tends to be farther from the disk at SKR longitudes around ˜140° and closer to it for longitudes around ˜320°. Depending on these factors, Titan is exposed to either: (i) a ‘magnetodisk lobe’ regime where the plasma beta is low and fields are radially ‘stretched’ and usually stronger or (ii) a ‘current sheet’ regime—characterized by quasi-dipolar, relatively weak fields and a high-beta plasma.
Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes 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. Imperial College London; Reino Unido
Fil: Sinclair, B.. Imperial College London; Reino Unido
Fil: Achilleos, N.. University College London; Estados Unidos
Fil: Hunt, P.. Imperial College London; Reino Unido
Fil: Dougherty, M. K.. Imperial College London; Reino Unido
Fil: Arridge, C. S.. University College London; Estados Unidos
description With a mean orbital radius of 20.2 Saturnian radii (1 Saturn radius RS=60,330 km), Titan is usually located within the kronian magnetosphere. 3.5 years of Cassini magnetometer observations in the vicinity of Titan´s orbit reveal that the moon´s magnetic environment is strongly affected by the presence of Saturn´s magnetodisk. As a result of the disk´s solar-wind-induced asymmetry, Titan is exposed to quasi-dipolar fields in the noon sector, and planetward, swept-back fields in the dawn, dusk and midnight sectors. These magnetic properties indicate that the moon is, on average, south of the central current sheet and immersed in Saturn´s rotating magnetospheric plasma for all local times (SLT). At a given SLT, Titan´s distance from the central current sheet associated with the magnetodisk depends on the solar wind pressure and on the phase of the Saturn´s kilometric radiation (SKR). The influence of the solar wind is present at all SLT (although dominant in the noon sector), whereas the SKR modulation seems to affect the magnetic field to first-order at least in the dawn sector. Near dawn local times, Titan tends to be farther from the disk at SKR longitudes around ˜140° and closer to it for longitudes around ˜320°. Depending on these factors, Titan is exposed to either: (i) a ‘magnetodisk lobe’ regime where the plasma beta is low and fields are radially ‘stretched’ and usually stronger or (ii) a ‘current sheet’ regime—characterized by quasi-dipolar, relatively weak fields and a high-beta plasma.
publishDate 2009
dc.date.none.fl_str_mv 2009-12
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/11336/20687
Bertucci, Cesar; Sinclair, B.; Achilleos, N.; Hunt, P.; Dougherty, M. K.; et al.; The variability of Titan's magnetic environment; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1813-1820
0032-0633
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20687
identifier_str_mv Bertucci, Cesar; Sinclair, B.; Achilleos, N.; Hunt, P.; Dougherty, M. K.; et al.; The variability of Titan's magnetic environment; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1813-1820
0032-0633
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2009.02.009
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063309000543
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Elsevier
publisher.none.fl_str_mv Elsevier
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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