Titan ionospheric conductivities from Cassini measurements

Autores
Rosenqvist, L.; Wahlund, J. E.; Ågren, K.; Modolo, R.; Opgenoorth, H. J.; Strobel, D.; Müller Wodarg, I.; Garnier, P.; Bertucci, Cesar
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
(approximately the location of the exobase) to approximately 1000 km where electrical currents perpendicular to the magnetic field may become important. In this region the ionosphere is highly conductive with peak Pedersen conductivities of 0.002–0.05 S/m and peak Hall conductivities of 0.01–0.3 S/m depending on Solar illumination and magnetospheric conditions. Ionospheric conductivities are found to be typically higher on the sunlit side of Titan. However, Hall and Pedersen conductivities depend strongly on the magnetic field magnitude which is highly variable, both in altitude and with respect to the draping configuration of Saturn's magnetic field around Titan. Furthermore, a consistent double peak nature is found in the altitude profile of the Pedersen conductivity. A high altitude peak is found to be located between 1300 and 1400 km. A second and typically more conductive region is observed below 1000 km, where the magnetic field strength drops sharply while the electron density still remains high. This nature of the Pedersen conductivity profile may give rise to complicated ionospheric–atmospheric dynamics and may be expected also at other unmagnetized objects with a substantial atmosphere, such as e.g. Mars and Venus. Estimates of the total Pedersen conductance are found to range between 1300 and 22,000 S. The Pedersen conductance is always higher than the local Alfvén conductance but the difference varies by two orders of magnitude (from a factor 4 to 100). Thus, the conditions for reflection or absorption of Alfvén waves in Titans ionosphere are highly variable and depends strongly on the magnetic field strength.
Fil: Rosenqvist, L.. Swedish Institute of Space Physics; Suecia
Fil: Wahlund, J. E.. Swedish Institute of Space Physics; Suecia
Fil: Ågren, K.. Swedish Institute of Space Physics; Suecia
Fil: Modolo, R.. Swedish Institute of Space Physics; Suecia
Fil: Opgenoorth, H. J.. Solar System Mission Division; Países Bajos
Fil: Strobel, D.. University Johns Hopkins; Estados Unidos
Fil: Müller Wodarg, I.. Imperial College London; Reino Unido
Fil: Garnier, P.. Swedish Institute of Space Physics; Suecia
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
Materia
Titan
Ionosphere
Cassini
Conductivity
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-nd/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/20679
Acceder
id CONICETDig_b45dfa06f52bedbdfa99c8e99f6e654b
oai_identifier_str oai:ri.conicet.gov.ar:11336/20679
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Titan ionospheric conductivities from Cassini measurementsRosenqvist, L.Wahlund, J. E.Ågren, K.Modolo, R.Opgenoorth, H. J.Strobel, D.Müller Wodarg, I.Garnier, P.Bertucci, CesarTitanIonosphereCassiniConductivityhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1(approximately the location of the exobase) to approximately 1000 km where electrical currents perpendicular to the magnetic field may become important. In this region the ionosphere is highly conductive with peak Pedersen conductivities of 0.002–0.05 S/m and peak Hall conductivities of 0.01–0.3 S/m depending on Solar illumination and magnetospheric conditions. Ionospheric conductivities are found to be typically higher on the sunlit side of Titan. However, Hall and Pedersen conductivities depend strongly on the magnetic field magnitude which is highly variable, both in altitude and with respect to the draping configuration of Saturn's magnetic field around Titan. Furthermore, a consistent double peak nature is found in the altitude profile of the Pedersen conductivity. A high altitude peak is found to be located between 1300 and 1400 km. A second and typically more conductive region is observed below 1000 km, where the magnetic field strength drops sharply while the electron density still remains high. This nature of the Pedersen conductivity profile may give rise to complicated ionospheric–atmospheric dynamics and may be expected also at other unmagnetized objects with a substantial atmosphere, such as e.g. Mars and Venus. Estimates of the total Pedersen conductance are found to range between 1300 and 22,000 S. The Pedersen conductance is always higher than the local Alfvén conductance but the difference varies by two orders of magnitude (from a factor 4 to 100). Thus, the conditions for reflection or absorption of Alfvén waves in Titans ionosphere are highly variable and depends strongly on the magnetic field strength.Fil: Rosenqvist, L.. Swedish Institute of Space Physics; SueciaFil: Wahlund, J. E.. Swedish Institute of Space Physics; SueciaFil: Ågren, K.. Swedish Institute of Space Physics; SueciaFil: Modolo, R.. Swedish Institute of Space Physics; SueciaFil: Opgenoorth, H. J.. Solar System Mission Division; Países BajosFil: Strobel, D.. University Johns Hopkins; Estados UnidosFil: Müller Wodarg, I.. Imperial College London; Reino UnidoFil: Garnier, P.. Swedish Institute of Space Physics; SueciaFil: 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; ArgentinaElsevier2009-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20679Rosenqvist, L.; Wahlund, J. E.; Ågren, K.; Modolo, R.; Opgenoorth, H. J.; et al.; Titan ionospheric conductivities from Cassini measurements; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1828-18330032-0633CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2009.01.007info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063309000233info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-nd/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:40:26Zoai:ri.conicet.gov.ar:11336/20679instacron: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:34982025-09-29 09:40:26.437CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Titan ionospheric conductivities from Cassini measurements
title Titan ionospheric conductivities from Cassini measurements
spellingShingle Titan ionospheric conductivities from Cassini measurements
Rosenqvist, L.
Titan
Ionosphere
Cassini
Conductivity
title_short Titan ionospheric conductivities from Cassini measurements
title_full Titan ionospheric conductivities from Cassini measurements
title_fullStr Titan ionospheric conductivities from Cassini measurements
title_full_unstemmed Titan ionospheric conductivities from Cassini measurements
title_sort Titan ionospheric conductivities from Cassini measurements
dc.creator.none.fl_str_mv Rosenqvist, L.
Wahlund, J. E.
Ågren, K.
Modolo, R.
Opgenoorth, H. J.
Strobel, D.
Müller Wodarg, I.
Garnier, P.
Bertucci, Cesar
author Rosenqvist, L.
author_facet Rosenqvist, L.
Wahlund, J. E.
Ågren, K.
Modolo, R.
Opgenoorth, H. J.
Strobel, D.
Müller Wodarg, I.
Garnier, P.
Bertucci, Cesar
author_role author
author2 Wahlund, J. E.
Ågren, K.
Modolo, R.
Opgenoorth, H. J.
Strobel, D.
Müller Wodarg, I.
Garnier, P.
Bertucci, Cesar
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Titan
Ionosphere
Cassini
Conductivity
topic Titan
Ionosphere
Cassini
Conductivity
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv (approximately the location of the exobase) to approximately 1000 km where electrical currents perpendicular to the magnetic field may become important. In this region the ionosphere is highly conductive with peak Pedersen conductivities of 0.002–0.05 S/m and peak Hall conductivities of 0.01–0.3 S/m depending on Solar illumination and magnetospheric conditions. Ionospheric conductivities are found to be typically higher on the sunlit side of Titan. However, Hall and Pedersen conductivities depend strongly on the magnetic field magnitude which is highly variable, both in altitude and with respect to the draping configuration of Saturn's magnetic field around Titan. Furthermore, a consistent double peak nature is found in the altitude profile of the Pedersen conductivity. A high altitude peak is found to be located between 1300 and 1400 km. A second and typically more conductive region is observed below 1000 km, where the magnetic field strength drops sharply while the electron density still remains high. This nature of the Pedersen conductivity profile may give rise to complicated ionospheric–atmospheric dynamics and may be expected also at other unmagnetized objects with a substantial atmosphere, such as e.g. Mars and Venus. Estimates of the total Pedersen conductance are found to range between 1300 and 22,000 S. The Pedersen conductance is always higher than the local Alfvén conductance but the difference varies by two orders of magnitude (from a factor 4 to 100). Thus, the conditions for reflection or absorption of Alfvén waves in Titans ionosphere are highly variable and depends strongly on the magnetic field strength.
Fil: Rosenqvist, L.. Swedish Institute of Space Physics; Suecia
Fil: Wahlund, J. E.. Swedish Institute of Space Physics; Suecia
Fil: Ågren, K.. Swedish Institute of Space Physics; Suecia
Fil: Modolo, R.. Swedish Institute of Space Physics; Suecia
Fil: Opgenoorth, H. J.. Solar System Mission Division; Países Bajos
Fil: Strobel, D.. University Johns Hopkins; Estados Unidos
Fil: Müller Wodarg, I.. Imperial College London; Reino Unido
Fil: Garnier, P.. Swedish Institute of Space Physics; Suecia
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
description (approximately the location of the exobase) to approximately 1000 km where electrical currents perpendicular to the magnetic field may become important. In this region the ionosphere is highly conductive with peak Pedersen conductivities of 0.002–0.05 S/m and peak Hall conductivities of 0.01–0.3 S/m depending on Solar illumination and magnetospheric conditions. Ionospheric conductivities are found to be typically higher on the sunlit side of Titan. However, Hall and Pedersen conductivities depend strongly on the magnetic field magnitude which is highly variable, both in altitude and with respect to the draping configuration of Saturn's magnetic field around Titan. Furthermore, a consistent double peak nature is found in the altitude profile of the Pedersen conductivity. A high altitude peak is found to be located between 1300 and 1400 km. A second and typically more conductive region is observed below 1000 km, where the magnetic field strength drops sharply while the electron density still remains high. This nature of the Pedersen conductivity profile may give rise to complicated ionospheric–atmospheric dynamics and may be expected also at other unmagnetized objects with a substantial atmosphere, such as e.g. Mars and Venus. Estimates of the total Pedersen conductance are found to range between 1300 and 22,000 S. The Pedersen conductance is always higher than the local Alfvén conductance but the difference varies by two orders of magnitude (from a factor 4 to 100). Thus, the conditions for reflection or absorption of Alfvén waves in Titans ionosphere are highly variable and depends strongly on the magnetic field strength.
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/11336/20679
Rosenqvist, L.; Wahlund, J. E.; Ågren, K.; Modolo, R.; Opgenoorth, H. J.; et al.; Titan ionospheric conductivities from Cassini measurements; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1828-1833
0032-0633
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20679
identifier_str_mv Rosenqvist, L.; Wahlund, J. E.; Ågren, K.; Modolo, R.; Opgenoorth, H. J.; et al.; Titan ionospheric conductivities from Cassini measurements; Elsevier; Planetary and Space Science; 57; 14-15; 12-2009; 1828-1833
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.2009.01.007
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063309000233
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-nd/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-nd/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 13.069144

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