Saturn's ULF wave foreshock boundary: Cassini observations

Autores
Andrés, Nahuel; Gomez, Daniel Osvaldo; Bertucci, Cesar; Mazelle, C.; Dougherty, M.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Even though the solar wind is highly supersonic, intense ultra-low frequency (ULF) wave activity has been detected in regions just upstream of the bow shocks of magnetized planets. This feature was first observed ahead of the Earth’s bow shock, and the corresponding region was called the ULF wave foreshock, which is embedded within the planet’s foreshock. The properties as well as the spatial distribution of ULF waves within the Earth’s foreshock have been extensively studied over the last three decades and have been explained as a result of plasma instabilities triggered by solar wind ions backstreaming from the bow shock. Since July 2004, the Cassini spacecraft has characterized the Saturnian plasma environment including its upstream region. Since Cassini’s Saturn orbit insertion (SOI) in June 2004 through August 2005, we conducted a detailed survey and analysis of observations made by the Vector Helium Magnetometer (VHM). The purpose of the present study is to characterize the properties of waves observed in Saturn’s ULF wave foreshock and identify its boundary using single spacecraft techniques. The amplitude of these waves is usually comparable to the mean magnetic field intensity, while their frequencies in the spacecraft frame yields two clearly different types of waves: one with frequencies below the local proton cyclotron frequency (OHþ ) and another with frequencies above OHþ . All the wave crossings described here, clearly show that these waves are associated to Saturn’s foreshock. In particular, the presence of waves is associated with the change in yBn to quasiparallel geometries. Our results show the existence of a clear boundary for Saturn’s ULF wave foreshock, compatible with yBn 451 surfaces.
Fil: Andrés, Nahuel. 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
Fil: Gomez, Daniel Osvaldo. 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
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
Fil: Mazelle, C.. Institut de Recherche en Astrophysique et Planetologie; Francia
Fil: Dougherty, M.. Imperial College Of Science And Technology; Reino Unido
Materia
Foreshock
Ulf Waves
Saturn
Cassini
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:11336/17080
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/17080
network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Saturn's ULF wave foreshock boundary: Cassini observationsAndrés, NahuelGomez, Daniel OsvaldoBertucci, CesarMazelle, C.Dougherty, M.ForeshockUlf WavesSaturnCassinihttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Even though the solar wind is highly supersonic, intense ultra-low frequency (ULF) wave activity has been detected in regions just upstream of the bow shocks of magnetized planets. This feature was first observed ahead of the Earth’s bow shock, and the corresponding region was called the ULF wave foreshock, which is embedded within the planet’s foreshock. The properties as well as the spatial distribution of ULF waves within the Earth’s foreshock have been extensively studied over the last three decades and have been explained as a result of plasma instabilities triggered by solar wind ions backstreaming from the bow shock. Since July 2004, the Cassini spacecraft has characterized the Saturnian plasma environment including its upstream region. Since Cassini’s Saturn orbit insertion (SOI) in June 2004 through August 2005, we conducted a detailed survey and analysis of observations made by the Vector Helium Magnetometer (VHM). The purpose of the present study is to characterize the properties of waves observed in Saturn’s ULF wave foreshock and identify its boundary using single spacecraft techniques. The amplitude of these waves is usually comparable to the mean magnetic field intensity, while their frequencies in the spacecraft frame yields two clearly different types of waves: one with frequencies below the local proton cyclotron frequency (OHþ ) and another with frequencies above OHþ . All the wave crossings described here, clearly show that these waves are associated to Saturn’s foreshock. In particular, the presence of waves is associated with the change in yBn to quasiparallel geometries. Our results show the existence of a clear boundary for Saturn’s ULF wave foreshock, compatible with yBn 451 surfaces.Fil: Andrés, Nahuel. 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; ArgentinaFil: Gomez, Daniel Osvaldo. 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; ArgentinaFil: 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; ArgentinaFil: Mazelle, C.. Institut de Recherche en Astrophysique et Planetologie; FranciaFil: Dougherty, M.. Imperial College Of Science And Technology; Reino UnidoElsevier2013-02-20info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/17080Andrés, Nahuel; Gomez, Daniel Osvaldo; Bertucci, Cesar; Mazelle, C.; Dougherty, M.; Saturn's ULF wave foreshock boundary: Cassini observations; Elsevier; Planetary And Space Science; 79-80; 20-2-2013; 64-750032-0633enginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2013.01.014info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063313000305info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-nd/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:46:09Zoai:ri.conicet.gov.ar:11336/17080instacron: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:34982025-09-03 09:46:10.572CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Saturn's ULF wave foreshock boundary: Cassini observations
title Saturn's ULF wave foreshock boundary: Cassini observations
spellingShingle Saturn's ULF wave foreshock boundary: Cassini observations
Andrés, Nahuel
Foreshock
Ulf Waves
Saturn
Cassini
title_short Saturn's ULF wave foreshock boundary: Cassini observations
title_full Saturn's ULF wave foreshock boundary: Cassini observations
title_fullStr Saturn's ULF wave foreshock boundary: Cassini observations
title_full_unstemmed Saturn's ULF wave foreshock boundary: Cassini observations
title_sort Saturn's ULF wave foreshock boundary: Cassini observations
dc.creator.none.fl_str_mv Andrés, Nahuel
Gomez, Daniel Osvaldo
Bertucci, Cesar
Mazelle, C.
Dougherty, M.
author Andrés, Nahuel
author_facet Andrés, Nahuel
Gomez, Daniel Osvaldo
Bertucci, Cesar
Mazelle, C.
Dougherty, M.
author_role author
author2 Gomez, Daniel Osvaldo
Bertucci, Cesar
Mazelle, C.
Dougherty, M.
author2_role author
author
author
author
dc.subject.none.fl_str_mv Foreshock
Ulf Waves
Saturn
Cassini
topic Foreshock
Ulf Waves
Saturn
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 Even though the solar wind is highly supersonic, intense ultra-low frequency (ULF) wave activity has been detected in regions just upstream of the bow shocks of magnetized planets. This feature was first observed ahead of the Earth’s bow shock, and the corresponding region was called the ULF wave foreshock, which is embedded within the planet’s foreshock. The properties as well as the spatial distribution of ULF waves within the Earth’s foreshock have been extensively studied over the last three decades and have been explained as a result of plasma instabilities triggered by solar wind ions backstreaming from the bow shock. Since July 2004, the Cassini spacecraft has characterized the Saturnian plasma environment including its upstream region. Since Cassini’s Saturn orbit insertion (SOI) in June 2004 through August 2005, we conducted a detailed survey and analysis of observations made by the Vector Helium Magnetometer (VHM). The purpose of the present study is to characterize the properties of waves observed in Saturn’s ULF wave foreshock and identify its boundary using single spacecraft techniques. The amplitude of these waves is usually comparable to the mean magnetic field intensity, while their frequencies in the spacecraft frame yields two clearly different types of waves: one with frequencies below the local proton cyclotron frequency (OHþ ) and another with frequencies above OHþ . All the wave crossings described here, clearly show that these waves are associated to Saturn’s foreshock. In particular, the presence of waves is associated with the change in yBn to quasiparallel geometries. Our results show the existence of a clear boundary for Saturn’s ULF wave foreshock, compatible with yBn 451 surfaces.
Fil: Andrés, Nahuel. 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
Fil: Gomez, Daniel Osvaldo. 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
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
Fil: Mazelle, C.. Institut de Recherche en Astrophysique et Planetologie; Francia
Fil: Dougherty, M.. Imperial College Of Science And Technology; Reino Unido
description Even though the solar wind is highly supersonic, intense ultra-low frequency (ULF) wave activity has been detected in regions just upstream of the bow shocks of magnetized planets. This feature was first observed ahead of the Earth’s bow shock, and the corresponding region was called the ULF wave foreshock, which is embedded within the planet’s foreshock. The properties as well as the spatial distribution of ULF waves within the Earth’s foreshock have been extensively studied over the last three decades and have been explained as a result of plasma instabilities triggered by solar wind ions backstreaming from the bow shock. Since July 2004, the Cassini spacecraft has characterized the Saturnian plasma environment including its upstream region. Since Cassini’s Saturn orbit insertion (SOI) in June 2004 through August 2005, we conducted a detailed survey and analysis of observations made by the Vector Helium Magnetometer (VHM). The purpose of the present study is to characterize the properties of waves observed in Saturn’s ULF wave foreshock and identify its boundary using single spacecraft techniques. The amplitude of these waves is usually comparable to the mean magnetic field intensity, while their frequencies in the spacecraft frame yields two clearly different types of waves: one with frequencies below the local proton cyclotron frequency (OHþ ) and another with frequencies above OHþ . All the wave crossings described here, clearly show that these waves are associated to Saturn’s foreshock. In particular, the presence of waves is associated with the change in yBn to quasiparallel geometries. Our results show the existence of a clear boundary for Saturn’s ULF wave foreshock, compatible with yBn 451 surfaces.
publishDate 2013
dc.date.none.fl_str_mv 2013-02-20
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/11336/17080
Andrés, Nahuel; Gomez, Daniel Osvaldo; Bertucci, Cesar; Mazelle, C.; Dougherty, M.; Saturn's ULF wave foreshock boundary: Cassini observations; Elsevier; Planetary And Space Science; 79-80; 20-2-2013; 64-75
0032-0633
url http://hdl.handle.net/11336/17080
identifier_str_mv Andrés, Nahuel; Gomez, Daniel Osvaldo; Bertucci, Cesar; Mazelle, C.; Dougherty, M.; Saturn's ULF wave foreshock boundary: Cassini observations; Elsevier; Planetary And Space Science; 79-80; 20-2-2013; 64-75
0032-0633
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.2013.01.014
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0032063313000305
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 13.13397

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