Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause
- Autores
- Foullon, C.; Farrugia, C. J.; Fazakerley, A. N.; Owen, C. J.; Gratton, Fausto Tulio Livio; Torbert, R.
- Año de publicación
- 2008
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Our purpose is to characterize the evolution of the magnetopause Kelvin-Helmholtz (KH) wave activity with changes in thickness of the adjacent boundary layer, geomagnetic latitude and interplanetary magnetic field (IMF) orientation. As the IMF turns northward, wave activity may be generated at the dayside before propagating down the tail, where the boundary layer is expected to support longer wavelengths. We use two-point observations on the dusk magnetopause at low latitudes, from Geotail on the dayside and Cluster tailward of the dusk terminator. We quantify the wavelength, power, wavefront steepness and propagation direction at Cluster. An estimate of the thickness of the low-latitude boundary layer (LLBL) is obtained by correlating normal distances to the magnetopause, derived from two empirical solar-wind-driven models, with a systematic relationship (the ‘‘transition parameter’’) found between the electron number density and temperature; the correlation factor is used to infer the temporal evolution of the thickness of the locally sampled layer. We find that wavelengths are controlled by the IMF clock angle, as expected when generated by the KH mechanism at the dayside, although amplitudes, wavefront steepness and propagation directions are more closely correlated with the layer thickness. A survey of parameter space provides evidence of the contribution of the KH mechanism to the widening of the electron LLBL.
Fil: Foullon, C.. University College London; Estados Unidos
Fil: Farrugia, C. J.. University of New Hampshire; Estados Unidos
Fil: Fazakerley, A. N.. University College London; Estados Unidos
Fil: Owen, C. J.. University College London; Estados Unidos
Fil: Gratton, Fausto Tulio Livio. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; Argentina
Fil: Torbert, R.. University of New Hampshire; Estados Unidos - Materia
-
KELVIN-HELMHOLTZ
MAGNETOPAUSE
ACTIVITY
FLANK - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/103417
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Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopauseFoullon, C.Farrugia, C. J.Fazakerley, A. N.Owen, C. J.Gratton, Fausto Tulio LivioTorbert, R.KELVIN-HELMHOLTZMAGNETOPAUSEACTIVITYFLANKhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Our purpose is to characterize the evolution of the magnetopause Kelvin-Helmholtz (KH) wave activity with changes in thickness of the adjacent boundary layer, geomagnetic latitude and interplanetary magnetic field (IMF) orientation. As the IMF turns northward, wave activity may be generated at the dayside before propagating down the tail, where the boundary layer is expected to support longer wavelengths. We use two-point observations on the dusk magnetopause at low latitudes, from Geotail on the dayside and Cluster tailward of the dusk terminator. We quantify the wavelength, power, wavefront steepness and propagation direction at Cluster. An estimate of the thickness of the low-latitude boundary layer (LLBL) is obtained by correlating normal distances to the magnetopause, derived from two empirical solar-wind-driven models, with a systematic relationship (the ‘‘transition parameter’’) found between the electron number density and temperature; the correlation factor is used to infer the temporal evolution of the thickness of the locally sampled layer. We find that wavelengths are controlled by the IMF clock angle, as expected when generated by the KH mechanism at the dayside, although amplitudes, wavefront steepness and propagation directions are more closely correlated with the layer thickness. A survey of parameter space provides evidence of the contribution of the KH mechanism to the widening of the electron LLBL.Fil: Foullon, C.. University College London; Estados UnidosFil: Farrugia, C. J.. University of New Hampshire; Estados UnidosFil: Fazakerley, A. N.. University College London; Estados UnidosFil: Owen, C. J.. University College London; Estados UnidosFil: Gratton, Fausto Tulio Livio. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; ArgentinaFil: Torbert, R.. University of New Hampshire; Estados UnidosAmerican Geophysical Union2008-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/103417Foullon, C.; Farrugia, C. J.; Fazakerley, A. N.; Owen, C. J.; Gratton, Fausto Tulio Livio; et al.; Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause; American Geophysical Union; Journal of Geophysical Research; 113; 11; 11-2008; 1-200148-0227CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013175info:eu-repo/semantics/altIdentifier/url/https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2008JA013175info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:53:02Zoai:ri.conicet.gov.ar:11336/103417instacron: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 09:53:02.968CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
title |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
spellingShingle |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause Foullon, C. KELVIN-HELMHOLTZ MAGNETOPAUSE ACTIVITY FLANK |
title_short |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
title_full |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
title_fullStr |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
title_full_unstemmed |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
title_sort |
Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause |
dc.creator.none.fl_str_mv |
Foullon, C. Farrugia, C. J. Fazakerley, A. N. Owen, C. J. Gratton, Fausto Tulio Livio Torbert, R. |
author |
Foullon, C. |
author_facet |
Foullon, C. Farrugia, C. J. Fazakerley, A. N. Owen, C. J. Gratton, Fausto Tulio Livio Torbert, R. |
author_role |
author |
author2 |
Farrugia, C. J. Fazakerley, A. N. Owen, C. J. Gratton, Fausto Tulio Livio Torbert, R. |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
KELVIN-HELMHOLTZ MAGNETOPAUSE ACTIVITY FLANK |
topic |
KELVIN-HELMHOLTZ MAGNETOPAUSE ACTIVITY FLANK |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Our purpose is to characterize the evolution of the magnetopause Kelvin-Helmholtz (KH) wave activity with changes in thickness of the adjacent boundary layer, geomagnetic latitude and interplanetary magnetic field (IMF) orientation. As the IMF turns northward, wave activity may be generated at the dayside before propagating down the tail, where the boundary layer is expected to support longer wavelengths. We use two-point observations on the dusk magnetopause at low latitudes, from Geotail on the dayside and Cluster tailward of the dusk terminator. We quantify the wavelength, power, wavefront steepness and propagation direction at Cluster. An estimate of the thickness of the low-latitude boundary layer (LLBL) is obtained by correlating normal distances to the magnetopause, derived from two empirical solar-wind-driven models, with a systematic relationship (the ‘‘transition parameter’’) found between the electron number density and temperature; the correlation factor is used to infer the temporal evolution of the thickness of the locally sampled layer. We find that wavelengths are controlled by the IMF clock angle, as expected when generated by the KH mechanism at the dayside, although amplitudes, wavefront steepness and propagation directions are more closely correlated with the layer thickness. A survey of parameter space provides evidence of the contribution of the KH mechanism to the widening of the electron LLBL. Fil: Foullon, C.. University College London; Estados Unidos Fil: Farrugia, C. J.. University of New Hampshire; Estados Unidos Fil: Fazakerley, A. N.. University College London; Estados Unidos Fil: Owen, C. J.. University College London; Estados Unidos Fil: Gratton, Fausto Tulio Livio. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; Argentina Fil: Torbert, R.. University of New Hampshire; Estados Unidos |
description |
Our purpose is to characterize the evolution of the magnetopause Kelvin-Helmholtz (KH) wave activity with changes in thickness of the adjacent boundary layer, geomagnetic latitude and interplanetary magnetic field (IMF) orientation. As the IMF turns northward, wave activity may be generated at the dayside before propagating down the tail, where the boundary layer is expected to support longer wavelengths. We use two-point observations on the dusk magnetopause at low latitudes, from Geotail on the dayside and Cluster tailward of the dusk terminator. We quantify the wavelength, power, wavefront steepness and propagation direction at Cluster. An estimate of the thickness of the low-latitude boundary layer (LLBL) is obtained by correlating normal distances to the magnetopause, derived from two empirical solar-wind-driven models, with a systematic relationship (the ‘‘transition parameter’’) found between the electron number density and temperature; the correlation factor is used to infer the temporal evolution of the thickness of the locally sampled layer. We find that wavelengths are controlled by the IMF clock angle, as expected when generated by the KH mechanism at the dayside, although amplitudes, wavefront steepness and propagation directions are more closely correlated with the layer thickness. A survey of parameter space provides evidence of the contribution of the KH mechanism to the widening of the electron LLBL. |
publishDate |
2008 |
dc.date.none.fl_str_mv |
2008-11 |
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/11336/103417 Foullon, C.; Farrugia, C. J.; Fazakerley, A. N.; Owen, C. J.; Gratton, Fausto Tulio Livio; et al.; Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause; American Geophysical Union; Journal of Geophysical Research; 113; 11; 11-2008; 1-20 0148-0227 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/103417 |
identifier_str_mv |
Foullon, C.; Farrugia, C. J.; Fazakerley, A. N.; Owen, C. J.; Gratton, Fausto Tulio Livio; et al.; Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause; American Geophysical Union; Journal of Geophysical Research; 113; 11; 11-2008; 1-20 0148-0227 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013175 info:eu-repo/semantics/altIdentifier/url/https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2008JA013175 |
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 application/pdf |
dc.publisher.none.fl_str_mv |
American Geophysical Union |
publisher.none.fl_str_mv |
American Geophysical Union |
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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1842269197189513216 |
score |
13.13397 |