Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation
International audience The aim of this study is to simulate the slow mode structures in the Hermean magnetosphere. We use a single fluid MHD model and a multipolar expansion of the Northward displaced Hermean magnetic field, to perform simulations with different solar wind parameters to foreseen the...
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ftobservparis:oai:HAL:hal-02320457v1 2024-06-09T07:49:36+00:00 Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation Varela, J. Pantellini, F. Moncuquet, M. Département d'Astrophysique (ex SAP) (DAP) Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU) Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA) Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS) Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA) Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris Université Paris Sciences et Lettres (PSL)-Université Paris Sciences et Lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS) 2016-06 https://hal.science/hal-02320457 https://doi.org/10.1016/j.pss.2016.02.015 en eng HAL CCSD Elsevier info:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2016.02.015 hal-02320457 https://hal.science/hal-02320457 BIBCODE: 2016P&SS.125.80V doi:10.1016/j.pss.2016.02.015 ISSN: 0032-0633 Planetary and Space Science https://hal.science/hal-02320457 Planetary and Space Science, 2016, 125, pp.80-86. ⟨10.1016/j.pss.2016.02.015⟩ "MHD simulations" "Mercury" "Magnetosphere" "Slow mode waves" "Astrophysics - Earth and Planetary Astrophysics" "Physics - Space Physics" [SDU]Sciences of the Universe [physics] [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] info:eu-repo/semantics/article Journal articles 2016 ftobservparis https://doi.org/10.1016/j.pss.2016.02.015 2024-05-16T11:30:56Z International audience The aim of this study is to simulate the slow mode structures in the Hermean magnetosphere. We use a single fluid MHD model and a multipolar expansion of the Northward displaced Hermean magnetic field, to perform simulations with different solar wind parameters to foreseen the most favorable configuration for the formation of slow modes, attending to the solar wind density, velocity, temperature and the interplanetary magnetic field orientation. If the interplanetary magnetic field is aligned with the Mercury-Sun direction, the magnetic axis of Mercury in the Northward direction or the planet orbital plane, slow mode structures are observed nearby the South pole. If the orientation is in the Sun-Mercury or Northward directions, slow mode structures are observed nearby the North pole, but smaller compared with the structures near the South pole. Increasing the density or the solar wind velocity avoids the formation of slow modes structures, not observed for a dynamic pressure larger than 6.25 ·10-9 Pa in the case of a Northward interplanetary magnetic field orientation, due to the enhancement of the bow shock compression. If the solar wind temperature increases, the slow mode structures are wider because the sonic Mach number is smaller and the bow shock is less compressed. Article in Journal/Newspaper South pole Archive de l'Observatoire de Paris (HAL) North Pole South Pole Planetary and Space Science 125 80 86 |
institution |
Open Polar |
collection |
Archive de l'Observatoire de Paris (HAL) |
op_collection_id |
ftobservparis |
language |
English |
topic |
"MHD simulations" "Mercury" "Magnetosphere" "Slow mode waves" "Astrophysics - Earth and Planetary Astrophysics" "Physics - Space Physics" [SDU]Sciences of the Universe [physics] [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] |
spellingShingle |
"MHD simulations" "Mercury" "Magnetosphere" "Slow mode waves" "Astrophysics - Earth and Planetary Astrophysics" "Physics - Space Physics" [SDU]Sciences of the Universe [physics] [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] Varela, J. Pantellini, F. Moncuquet, M. Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
topic_facet |
"MHD simulations" "Mercury" "Magnetosphere" "Slow mode waves" "Astrophysics - Earth and Planetary Astrophysics" "Physics - Space Physics" [SDU]Sciences of the Universe [physics] [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] |
description |
International audience The aim of this study is to simulate the slow mode structures in the Hermean magnetosphere. We use a single fluid MHD model and a multipolar expansion of the Northward displaced Hermean magnetic field, to perform simulations with different solar wind parameters to foreseen the most favorable configuration for the formation of slow modes, attending to the solar wind density, velocity, temperature and the interplanetary magnetic field orientation. If the interplanetary magnetic field is aligned with the Mercury-Sun direction, the magnetic axis of Mercury in the Northward direction or the planet orbital plane, slow mode structures are observed nearby the South pole. If the orientation is in the Sun-Mercury or Northward directions, slow mode structures are observed nearby the North pole, but smaller compared with the structures near the South pole. Increasing the density or the solar wind velocity avoids the formation of slow modes structures, not observed for a dynamic pressure larger than 6.25 ·10-9 Pa in the case of a Northward interplanetary magnetic field orientation, due to the enhancement of the bow shock compression. If the solar wind temperature increases, the slow mode structures are wider because the sonic Mach number is smaller and the bow shock is less compressed. |
author2 |
Département d'Astrophysique (ex SAP) (DAP) Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU) Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Direction de Recherche Fondamentale (CEA) (DRF (CEA)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA) Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)) Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS) Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA) Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris Université Paris Sciences et Lettres (PSL)-Université Paris Sciences et Lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS) |
format |
Article in Journal/Newspaper |
author |
Varela, J. Pantellini, F. Moncuquet, M. |
author_facet |
Varela, J. Pantellini, F. Moncuquet, M. |
author_sort |
Varela, J. |
title |
Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
title_short |
Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
title_full |
Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
title_fullStr |
Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
title_full_unstemmed |
Slow modes in the Hermean magnetosphere: Effect of the solar wind hydrodynamic parameters and IMF orientation |
title_sort |
slow modes in the hermean magnetosphere: effect of the solar wind hydrodynamic parameters and imf orientation |
publisher |
HAL CCSD |
publishDate |
2016 |
url |
https://hal.science/hal-02320457 https://doi.org/10.1016/j.pss.2016.02.015 |
geographic |
North Pole South Pole |
geographic_facet |
North Pole South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
ISSN: 0032-0633 Planetary and Space Science https://hal.science/hal-02320457 Planetary and Space Science, 2016, 125, pp.80-86. ⟨10.1016/j.pss.2016.02.015⟩ |
op_relation |
info:eu-repo/semantics/altIdentifier/doi/10.1016/j.pss.2016.02.015 hal-02320457 https://hal.science/hal-02320457 BIBCODE: 2016P&SS.125.80V doi:10.1016/j.pss.2016.02.015 |
op_doi |
https://doi.org/10.1016/j.pss.2016.02.015 |
container_title |
Planetary and Space Science |
container_volume |
125 |
container_start_page |
80 |
op_container_end_page |
86 |
_version_ |
1801382307919036416 |