On The Nature of Turbulent Heating and Radial Transport in Saturn's Magnetosphere

Neupane, B. R.; Delamere, P. A.; Ma, Xuanye; Ng, C. S.; Burkholder, Brandon; Damiano, P. A.

doi:10.1029/2020ja027986

Cited by 9 publications

(38 citation statements)

References 44 publications

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“…Also of note, dayside field deflections from the catalog, while not validated, seem to be observed across a broader range of latitude and longitude with notable hotspots at

\pm 40 °

. These hotspots conform to the nonequatorial disturbed magnetic field events of (Neupane et al., 2021), however, they observed a more uniform distribution with latitude. Alternatively, these hotspots may be the most prominent location for magnetic flux tube twisting that facilitates the double reconnection process at mid latitudes from (Ma et al., 2019).…”

Section: Discussionmentioning

confidence: 73%

Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime

2021

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“…Also of note, dayside field deflections from the catalog, while not validated, seem to be observed across a broader range of latitude and longitude with notable hotspots at

\pm 40 °

Section: Discussionmentioning

confidence: 73%

Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime

2021

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“…A possible dissipation mode could be ion cyclotron damping in particular of the heavy sulfur and oxygen ions of Jupiter's magnetosphere (Saur et al, 2018). In Saturn's magnetosphere the dissipation of the magnetic field fluctuations based on a strong turbulence model could provide power on the order of 10 11 W (von Papen and Saur, 2016;Kaminker et al, 2017;Neupane et al, 2021), which is roughly consistent with the energy needed to heat the magnetosphere to its observed temperatures (Bagenal and Delamere, 2011).…”

Section: Magnetospheric Heatingmentioning

confidence: 70%

Turbulence in the Magnetospheres of the Outer Planets

Saur

2021

Front. Astron. Space Sci.

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The magnetospheres of the outer planets exhibit turbulent phenomena in an environment which is qualitatively different compared to the solar wind or the interstellar medium. The key differences are the finite sizes of the magnetospheres limited by their physical boundaries, the presence of a strong planetary background magnetic field and spatially very inhomogeneous plasma properties within the magnetospheres. Typical turbulent fluctuations possess amplitudes much smaller than the background field and are characterized by Alfvén times, which can be smaller than the non-linear interaction time scales. The magnetospheres of the outer planets are thus interesting laboratories of plasma turbulence. In Jupiter's and Saturn's magnetospheres, turbulence is well-established thanks to the in-situ measurements by several spacecraft, in particular the Galileo and Cassini orbiter. In contrast, the fluctuations in Uranus' and Neptune's magnetospheres are poorly understood due to the lack of sufficient data. Turbulence in the outer planets' magnetospheres have important effects on the systems as a whole. The dissipation of the turbulent fluctuations through wave-particle interaction is a significant heat source, which can explain the large magnetospheric plasma temperatures. Similarly, turbulent wave fluctuations strongly contribute to the acceleration of particles responsible for the planet's auroras.

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“…They found a quiet region between 3 and 9 LT and an active region between 10 and 20 LT with an average two orders of magnitude difference in q. We use the Ng et al (2018) advective turbulent heating model based to calculate the ion temperature, similar to Neupane et al (2021) but incorporating a local time asymmetry. The temperature is given by…”

Section: Discussionmentioning

confidence: 99%

“…kg is the mass transport rate (Neupane et al, 2021). We fix the parameters for both local time sectors but vary q based on Kaminker et al (2017) such that q ∼ 10 −16 W/m 3 at dusk and q ∼ 10 −18 W/m 3 at dawn.…”

Section: Discussionmentioning

confidence: 99%

The Cushion Region and Dayside Magnetodisc Structure at Saturn

Staniland

Dougherty

Masters

et al. 2021

Geophysical Research Letters

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At the gas giants, the presence of an internal plasma source coupled with their rapid rotation (∼10 h) significantly perturbs their magnetic field configuration. Neutrals ejected from the moons Enceladus and Io in the inner magnetosphere of Saturn and Jupiter, respectively, become ionized, locking onto magnetic field lines and are accelerated toward corotation. The newly formed plasma is centrifugally confined to the equator, radially stretching the magnetic field into a magnetodisc. This structure has been observed at all local times under expanded conditions at Saturn (Arridge, Russell, et al., 2008). At Jupiter, a region adjacent to the magnetopause where the magnetodisc structure breaks down and the field is quasi-dipolar, referred to as the "cushion region," has been identified (Went, Kivelson, et al., 2011) and is argued to be populated by mass-depleted flux tubes following tail reconnection (Kivelson & Southwood, 2005). However, this region has yet to be identified at Saturn (Went, Kivelson, et al., 2011), despite the similarities between these two systems. At Saturn, mass that is loaded into the magnetosphere by Enceladus must be lost from the system. These water group ions (W +) are eventually driven radially outwards in the low plasma beta (β < 1) inner magnetosphere via an interchange instability with the more tenuous hot plasma population in the outer magnetosphere (e.g., Azari et al., 2018; Gold, 1959). At larger radial distances, plasma pressure dominates (β > 1) and the magnetic field balloons until closed field lines reconnect and mass is lost in the magnetotail (Vasyliunas, 1983). Hence, mass-depleted flux tubes following nightside reconnection via this cycle, or the solar-wind driven Dungey cycle (Dungey, 1961), convect along the dawn flank toward noon and are subsequently refilled, thus restarting the mass transport cycle. It has been suggested that a turbulent channel

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On The Nature of Turbulent Heating and Radial Transport in Saturn's Magnetosphere

Cited by 9 publications

References 44 publications

Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime

Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime

Turbulence in the Magnetospheres of the Outer Planets

The Cushion Region and Dayside Magnetodisc Structure at Saturn

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