Local time asymmetry of Saturn's magnetosheath flows
Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postn...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
B Burkholder [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2017 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Geophysical research letters - Washington, DC : Union, 1974, 44(2017), 12, Seite 5877 |
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| Übergeordnetes Werk: |
volume:44 ; year:2017 ; number:12 ; pages:5877 |
| Links: |
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| DOI / URN: |
10.1002/2017GL073031 |
|---|
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| 520 | |a Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. | ||
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| 650 | 4 | |a Lines | |
| 650 | 4 | |a Solar wind | |
| 650 | 4 | |a Saturn's magnetosphere | |
| 650 | 4 | |a Kelvin-Helmholtz instability | |
| 650 | 4 | |a Stability | |
| 650 | 4 | |a Magnetism | |
| 650 | 4 | |a Magnetopause | |
| 650 | 4 | |a Drag | |
| 650 | 4 | |a Magnetospheres | |
| 650 | 4 | |a Saturn | |
| 650 | 4 | |a Magnetic fields | |
| 650 | 4 | |a Magnetosphere | |
| 650 | 4 | |a Tensor analysis | |
| 650 | 4 | |a Asymmetry | |
| 650 | 4 | |a Drag (hindrance) | |
| 650 | 4 | |a Planetary magnetospheres | |
| 650 | 4 | |a Magnetosheath | |
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10.1002/2017GL073031 doi PQ20170721 (DE-627)OLC1994204001 (DE-599)GBVOLC1994204001 (PRQ)p571-b5240c07060fd41ed0ec14840822e9a197e06ef4a76d7b683d1b780fa4dcf93c0 (KEY)0026932820170000044001205877localtimeasymmetryofsaturnsmagnetosheathflows DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl B Burkholder verfasserin aut Local time asymmetry of Saturn's magnetosheath flows 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability P A Delamere oth X Ma oth M F Thomsen oth R J Wilson oth F Bagenal oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 44(2017), 12, Seite 5877 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:44 year:2017 number:12 pages:5877 http://dx.doi.org/10.1002/2017GL073031 Volltext https://search.proquest.com/docview/1919462041 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 44 2017 12 5877 |
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10.1002/2017GL073031 doi PQ20170721 (DE-627)OLC1994204001 (DE-599)GBVOLC1994204001 (PRQ)p571-b5240c07060fd41ed0ec14840822e9a197e06ef4a76d7b683d1b780fa4dcf93c0 (KEY)0026932820170000044001205877localtimeasymmetryofsaturnsmagnetosheathflows DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl B Burkholder verfasserin aut Local time asymmetry of Saturn's magnetosheath flows 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability P A Delamere oth X Ma oth M F Thomsen oth R J Wilson oth F Bagenal oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 44(2017), 12, Seite 5877 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:44 year:2017 number:12 pages:5877 http://dx.doi.org/10.1002/2017GL073031 Volltext https://search.proquest.com/docview/1919462041 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 44 2017 12 5877 |
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10.1002/2017GL073031 doi PQ20170721 (DE-627)OLC1994204001 (DE-599)GBVOLC1994204001 (PRQ)p571-b5240c07060fd41ed0ec14840822e9a197e06ef4a76d7b683d1b780fa4dcf93c0 (KEY)0026932820170000044001205877localtimeasymmetryofsaturnsmagnetosheathflows DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl B Burkholder verfasserin aut Local time asymmetry of Saturn's magnetosheath flows 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability P A Delamere oth X Ma oth M F Thomsen oth R J Wilson oth F Bagenal oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 44(2017), 12, Seite 5877 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:44 year:2017 number:12 pages:5877 http://dx.doi.org/10.1002/2017GL073031 Volltext https://search.proquest.com/docview/1919462041 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 44 2017 12 5877 |
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10.1002/2017GL073031 doi PQ20170721 (DE-627)OLC1994204001 (DE-599)GBVOLC1994204001 (PRQ)p571-b5240c07060fd41ed0ec14840822e9a197e06ef4a76d7b683d1b780fa4dcf93c0 (KEY)0026932820170000044001205877localtimeasymmetryofsaturnsmagnetosheathflows DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl B Burkholder verfasserin aut Local time asymmetry of Saturn's magnetosheath flows 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability P A Delamere oth X Ma oth M F Thomsen oth R J Wilson oth F Bagenal oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 44(2017), 12, Seite 5877 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:44 year:2017 number:12 pages:5877 http://dx.doi.org/10.1002/2017GL073031 Volltext https://search.proquest.com/docview/1919462041 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 44 2017 12 5877 |
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10.1002/2017GL073031 doi PQ20170721 (DE-627)OLC1994204001 (DE-599)GBVOLC1994204001 (PRQ)p571-b5240c07060fd41ed0ec14840822e9a197e06ef4a76d7b683d1b780fa4dcf93c0 (KEY)0026932820170000044001205877localtimeasymmetryofsaturnsmagnetosheathflows DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl B Burkholder verfasserin aut Local time asymmetry of Saturn's magnetosheath flows 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability P A Delamere oth X Ma oth M F Thomsen oth R J Wilson oth F Bagenal oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 44(2017), 12, Seite 5877 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:44 year:2017 number:12 pages:5877 http://dx.doi.org/10.1002/2017GL073031 Volltext https://search.proquest.com/docview/1919462041 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 44 2017 12 5877 |
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Enthalten in Geophysical research letters 44(2017), 12, Seite 5877 volume:44 year:2017 number:12 pages:5877 |
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Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability |
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B Burkholder @@aut@@ P A Delamere @@oth@@ X Ma @@oth@@ M F Thomsen @@oth@@ R J Wilson @@oth@@ F Bagenal @@oth@@ |
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550 DNB 38.70 bkl Local time asymmetry of Saturn's magnetosheath flows Momentum Lines Solar wind Saturn's magnetosphere Kelvin-Helmholtz instability Stability Magnetism Magnetopause Drag Magnetospheres Saturn Magnetic fields Magnetosphere Tensor analysis Asymmetry Drag (hindrance) Planetary magnetospheres Magnetosheath Fluid flow Instability |
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Local time asymmetry of Saturn's magnetosheath flows |
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local time asymmetry of saturn's magnetosheath flows |
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Local time asymmetry of Saturn's magnetosheath flows |
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Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. |
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Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. |
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Using gross averages of the azimuthal component of flow in Saturn's magnetosheath, we find that flows in the prenoon sector reach a maximum value of roughly half that of the postnoon side. Corotational magnetodisc plasma creates a much larger flow shear with solar wind plasma prenoon than postnoon. Maxwell stress tensor analysis shows that momentum can be transferred out of the magnetosphere along tangential field lines if a normal component to the boundary is present, i.e., field lines which pierce the magnetopause. A Kelvin-Helmholtz unstable flow gives rise to precisely this situation, as intermittent reconnection allows the magnetic field to thread the boundary. We interpret the Kelvin-Helmholtz instability acting along the magnetopause as a tangetial drag, facilitating two-way transport of momentum through the boundary. We use reduced magnetosheath flows in the dawn sector as evidence of the importance of this interaction in Saturn's magnetosphere. |
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Local time asymmetry of Saturn's magnetosheath flows |
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