Properties of the boundary layer potential for northward interplanetary magnetic field

Sundberg, K. Å. T.; Blomberg, Lars G.; Cumnock, J. A.

doi:10.1029/2009gl038625

Cited by 9 publications

(7 citation statements)

References 41 publications

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“…Above 3 nT B z , the viscous potential is seen to settle asymptotically around 10 kV for the solar wind speed and density of 400 km/s and 5/cm 3 , whereas, for higher solar wind speed, the viscous potential settles at 10 kV for higher B z value, typically around 5–7 nT. Sundberg et al [] also determined an average boundary layer potential of 10 kV when they did a statistical study of 271 events with northward IMF using the DMSP‐F13 satellite. They also found that the boundary layer potential depends on viscous parameters such as the solar wind velocity, density, and ram pressure.…”

Section: Reduction Of the Viscous Potential In The Lfm Simulationmentioning

confidence: 99%

Reduction of viscous potential for northward interplanetary magnetic field as seen in the LFM simulation

Bhattarai

López

2013

JGR Space Physics

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[1] The two primary methods responsible for solar wind magnetosphere coupling are magnetic reconnection and the viscous interaction. The viscous interaction is generated due to the antisunward dragging of plasma inside the magnetopause by the plasma flowing in the magnetosheath, creating a return flow deeper inside the magnetosphere and producing a circulation pattern. This viscous circulation pattern is mapped into the ionosphere via magnetic field lines, which results in ionospheric electric field in the nonrotating Earth's frame. We measure this interaction in terms of an electric potential, the viscous potential. In this paper, we use the results obtained from the Lyon-Fedder-Mobarry (LFM) simulation model during periods of purely northward interplanetary magnetic field (IMF) for different solar wind velocity and ionospheric conductivity, showing a reduction of the viscous potential with increasing magnitude of northward IMF. The viscous potential is found to settle around 5-10 kV for large +B z values. The decrease in viscous potential was found to be associated with a weak or nonexistent sunward plasma flow in the nightside plasmasheet. Instead, the return flow to the dayside occurs at high latitudes and is associated with the reconnection topology and dynamics that occur during northward IMF periods. We also show that the magnetosphere remains closed during purely northward IMF, except for two small regions-one on each hemisphere, where the magnetic reconnection occur. We argue that the reduction of the viscous potential is due to a reduction of the velocity shear across the magnetopause and the lack of sunward convection in the equatorial tail.Citation: Bhattarai, S. K., and R. E. Lopez (2013), Reduction of viscous potential for northward interplanetary magnetic field as seen in the LFM simulation,

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Section: Reduction Of the Viscous Potential In The Lfm Simulationmentioning

confidence: 99%

Reduction of viscous potential for northward interplanetary magnetic field as seen in the LFM simulation

Bhattarai

López

2013

JGR Space Physics

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“…While the Newell et al (2008) state variables did not include CPCP, it is reasonable to surmise that the viscous potential varies as the viscous coupling term that they found. Sundberg et al (2009) identified the boundary layer convection cells during northward IMF, when the 4-cell convection pattern makes it possible to separate the viscous and merging convection in the ionosphere. They found a mean value of 9.8 kV for the boundary layer potential, and that this value correlated best with n 1/2 V 2 of those items that they tested.…”

Section: Introductionmentioning

confidence: 99%

Investigating the viscous interaction and its role in generating the ionospheric potential during the Whole Heliosphere Interval

Bruntz

López

Bhattarai

et al. 2012

Journal of Atmospheric and Solar-Terrestrial Physics

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“…Widespread evidence for ongoing reconnection at Earth's magnetopause at loci of points that describe reconnection “X‐lines” and comparison of cross‐polar potential measurements with theory has shown that the primary contributor to the potential is this global magnetic reconnection (applying between order 10 and order 100 kV), which is therefore thought to be the dominant driver of convection (e.g., Burch & Phan, ; Milan et al, ; Paschmann et al, ; Phan et al, ; Reiff et al, ; Russell & Elphic, ). There is also evidence for a secondary contribution to the cross‐polar potential of order 10 kV, which has been attributed to the viscous‐like interaction (e.g., Boyle et al, ; Bruntz et al, ; Reiff et al, ; Sundberg et al, ).…”

Section: Introductionmentioning

confidence: 99%

A More Viscous‐Like Solar Wind Interaction With All the Giant Planets

Masters

2018

Geophysical Research Letters

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Identifying and quantifying the different drivers of energy flow through a planetary magnetosphere is crucial for understanding how each planetary system works. The magnetosphere of our own planet is primarily driven externally by the solar wind through global magnetic reconnection, while a viscous‐like interaction with the solar wind involving growth of the Kelvin‐Helmholtz (K‐H) instability is a secondary effect. Here we consider the solar wind‐magnetosphere interaction at all magnetized planets, exploring the implications of diverse solar wind conditions. We show that with increasing distance from the Sun the electric fields arising from reconnection at the magnetopause boundary of a planetary magnetosphere become weaker, whereas the boundaries become increasingly K‐H unstable. Our results support the possibility of a predominantly viscous‐like interaction between the solar wind and every one of the giant planet magnetospheres, as proposed by previous authors and in contrast with the solar wind‐magnetosphere interaction at Earth.

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Properties of the boundary layer potential for northward interplanetary magnetic field

Cited by 9 publications

References 41 publications

Reduction of viscous potential for northward interplanetary magnetic field as seen in the LFM simulation

Reduction of viscous potential for northward interplanetary magnetic field as seen in the LFM simulation

Investigating the viscous interaction and its role in generating the ionospheric potential during the Whole Heliosphere Interval

A More Viscous‐Like Solar Wind Interaction With All the Giant Planets

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