Slow modes in the Hermean magnetosphere: effect of the solar wind hydrodynamic parameters and IMF orientation
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 parameter to foreseen the most favorable configur...
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ftdatacite:10.48550/arxiv.1608.04417 2023-05-15T18:22:06+02:00 Slow modes in the Hermean magnetosphere: effect of the solar wind hydrodynamic parameters and IMF orientation Varela, J. Pantellini, F. Moncuquet, M. 2016 https://dx.doi.org/10.48550/arxiv.1608.04417 https://arxiv.org/abs/1608.04417 unknown arXiv https://dx.doi.org/10.1016/j.pss.2016.02.015 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Earth and Planetary Astrophysics astro-ph.EP Space Physics physics.space-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2016 ftdatacite https://doi.org/10.48550/arxiv.1608.04417 https://doi.org/10.1016/j.pss.2016.02.015 2022-04-01T11:08:42Z 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 parameter 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. Increase the density or the solar wind velocity avoids the formation of slow modes structures, not observed for a dynamic pressure larger than $6.25 \cdot 10^{-9}$ 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. Text South pole DataCite Metadata Store (German National Library of Science and Technology) North Pole South Pole |
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Earth and Planetary Astrophysics astro-ph.EP Space Physics physics.space-ph FOS Physical sciences |
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Earth and Planetary Astrophysics astro-ph.EP Space Physics physics.space-ph FOS Physical sciences Varela, J. Pantellini, F. Moncuquet, M. Slow modes in the Hermean magnetosphere: effect of the solar wind hydrodynamic parameters and IMF orientation |
topic_facet |
Earth and Planetary Astrophysics astro-ph.EP Space Physics physics.space-ph FOS Physical sciences |
description |
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 parameter 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. Increase the density or the solar wind velocity avoids the formation of slow modes structures, not observed for a dynamic pressure larger than $6.25 \cdot 10^{-9}$ 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. |
format |
Text |
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 |
arXiv |
publishDate |
2016 |
url |
https://dx.doi.org/10.48550/arxiv.1608.04417 https://arxiv.org/abs/1608.04417 |
geographic |
North Pole South Pole |
geographic_facet |
North Pole South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1016/j.pss.2016.02.015 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1608.04417 https://doi.org/10.1016/j.pss.2016.02.015 |
_version_ |
1766201448609087488 |