Reconnection at the magnetopause of Saturn: Perspective from FTE occurrence and magnetosphere size

Lai, Hairong; Wei, H. Y.; Russell, C. T.; Arridge, C. S.; Dougherty, M. K.

doi:10.1029/2011ja017263

Cited by 52 publications

(67 citation statements)

References 33 publications

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“…An investigation of Cassini measurements in Saturn's magnetosheath by Masters et al (2014) found that in this case there is no difference in the plasma depletion layer for northward and southward IMF, which is contrary to the results of related Voyager measurements that indicated an IMF effect (Violante et al, 1995). Masters et al (2014) inferred that reconnection at the dayside magnetopause is not effective at Saturn. We emphasize that this may concern only northward IMF conditions, but not necessarily southward IMF conditions.…”

Section: Southward and Northward Imfcontrasting

confidence: 45%

“…The magnetic flux transport rate due to reconnection in this case appears to be lower than the rate of magnetic flux advection due to the solar wind flow. This may imply that conditions for magnetopause reconnection are less favorable at Saturn compared to those at the Earth (Masters et al, 2014).…”

Section: Introductionmentioning

confidence: 79%

“…Scurry and Russell (1991) suggested that the reconnection efficiency near Saturn is low due to the usual high magnetosonic Mach number of the solar wind flow at these distances, though this conclusion has been disputed by Grocott et al (2009). For related reasons, Masters et al (2014) have expressed doubt about the importance of reconnection at Saturn's magnetopause. They noted that despite reconnection signatures being observed in Saturn's magnetosphere (e.g., McAndrews et al, 2008;Radioti et al, 2011Radioti et al, , 2013Badman et al, 2013), the reconnection efficiency at Saturn may be much lower than at Earth due to the different solar wind conditions at these planets.…”

Section: Introductionmentioning

confidence: 93%

“…On the noon magnetopause FTEs could arise for northward IMF conditions. The absence of FTE observations at Saturn's noon magnetopause (as reported, e.g., by Huddleston et al, 1997;Lai et al, 2012) could mean that the partially closed magnetosphere model may be realized for northward IMF. According to Fig.…”

Section: Southward and Northward Imfmentioning

confidence: 99%

“…Thus, the conclusions of Masters et al (2014) do not mean that the reconnection in cusps, which is characteristic of southward IMF conditions, is not effective at Saturn. Masters et al (2014) noted that contrary to the case of Earth, magnetosheath flow is predominant over Saturn's poles due to magnetospheric flattening. In this situation the role of cusp reconnection for southward IMF could be enhanced at Saturn.…”

Section: Southward and Northward Imfmentioning

confidence: 99%

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Open and partially closed models of the solar wind interaction with outer planet magnetospheres: the case of Saturn

et al. 2017

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Abstract. A wide variety of interactions take place between the magnetized solar wind plasma outflow from the Sun and celestial bodies within the solar system. Magnetized planets form magnetospheres in the solar wind, with the planetary field creating an obstacle in the flow. The reconnection efficiency of the solar-wind-magnetized planet interaction depends on the conditions in the magnetized plasma flow passing the planet. When the reconnection efficiency is very low, the interplanetary magnetic field (IMF) does not penetrate the magnetosphere, a condition that has been widely discussed in the recent literature for the case of Saturn. In the present paper, we study this issue for Saturn using Cassini magnetometer data, images of Saturn's ultraviolet aurora obtained by the HST, and the paraboloid model of Saturn's magnetospheric magnetic field. Two models are considered: first, an open model in which the IMF penetrates the magnetosphere, and second, a partially closed model in which field lines from the ionosphere go to the distant tail and interact with the solar wind at its end. We conclude that the open model is preferable, which is more obvious for southward IMF. For northward IMF, the model calculations do not allow us to reach definite conclusions. However, analysis of the observations available in the literature provides evidence in favor of the open model in this case too. The difference in magnetospheric structure for these two IMF orientations is due to the fact that the reconnection topology and location depend on the relative orientation of the IMF vector and the planetary dipole magnetic moment. When these vectors are parallel, two-dimensional reconnection occurs at the low-latitude neutral line. When they are antiparallel, three-dimensional reconnection takes place in the cusp regions. Different magnetospheric topologies determine different mapping of the open-closed boundary in the ionosphere, which can be considered as a proxy for the poleward edge of the auroral oval.

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Section: Southward and Northward Imfcontrasting

confidence: 45%

Section: Introductionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 93%

Section: Southward and Northward Imfmentioning

confidence: 99%

Section: Southward and Northward Imfmentioning

confidence: 99%

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Open and partially closed models of the solar wind interaction with outer planet magnetospheres: the case of Saturn

et al. 2017

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Saturn's magnetospheric dynamics

Thomsen

2013

Geophysical Research Letters

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The dynamics of Saturn's magnetosphere are driven by two major features of the system: First, the dominant source of magnetospheric plasma is the icy moon Enceladus, located deep within the magnetosphere; and second, like Jupiter, Saturn is a very fast rotator, with a rotational period of only 10.7 h. The dynamical imperative is to rid the magnetosphere of the continuously supplied plasma, and the fast rotation provides the mechanisms to do so. Thus, magnetospheric dynamics are intimately related to mass transport processes, including radial diffusion, flux tube interchange, magnetic reconnection, and plasmoid formation. We review recent progress and new questions relating to these processes at Saturn.

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Magnetotail structure of the giant magnetospheres: Implications of the viscous interaction with the solar wind

Delamere

Bagenal

2013

JGR Space Physics

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[1] The internal sources of plasma in the giant magnetospheres of Jupiter and Saturn affect magnetospheric dynamics in terms of magnetosphere-ionosphere coupling and auroral current systems, as well as the interaction with the solar wind. The radial transport of plasma at Jupiter is well constrained to vary between 300 kg/s and 1200 kg/s over timescales of 20-60 days. Saturn's neutral-dominated inner magnetosphere has presented a challenge for determining the radial mass transport rates with values ranging between 20 kg/s and 280 kg/s over timescales of 20-80 days. We present an estimate of the radial mass transport rates associated with magnetospheric plasma production for Jupiter and Saturn, assuming that magnetospheric plasma loss (equal to the plasma source) can be treated as mass pickup by the solar wind. That is, the magnetospheric plasma is assumed to be at rest with respect to the solar wind, analogous to cometary mass loading of the solar wind flow. This Alfvénic coupling between the solar wind and the magnetosphere suggests mass loading rates of 500-1500 kg/s for Jupiter and 20-50 kg/s for Saturn, consistent with observations and physical chemistry models. We discuss implications for magnetotail structure by considering the contribution of the viscous interaction of the solar wind with the giant magnetospheres. We suggest that a significant portion of the magnetotail structure can be attributed to this viscous interaction.Citation: Delamere, P. A., and F. Bagenal (2013), Magnetotail structure of the giant magnetospheres: Implications of the viscous interaction with the solar wind,

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Reconnection at the magnetopause of Saturn: Perspective from FTE occurrence and magnetosphere size

Cited by 52 publications

References 33 publications

Open and partially closed models of the solar wind interaction with outer planet magnetospheres: the case of Saturn

Open and partially closed models of the solar wind interaction with outer planet magnetospheres: the case of Saturn

Saturn's magnetospheric dynamics

Magnetotail structure of the giant magnetospheres: Implications of the viscous interaction with the solar wind

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