Polar Flattening of Jupiter's Magnetosphere

Ranquist, D. A.; Bagenal, F.; Wilson, R.

doi:10.1029/2020gl089818

Cited by 4 publications

(5 citation statements)

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“…The spacecraft was in the magnetotail at radial distances of 109 and 107 R J and local times of 03:30 and 02:30, respectively. The Juno orbit had precessed south over these dozen orbits but these crossings at 16° and 21° south latitude support the idea of a flattened shape for the magnetopause (Ranquist et al, 2020) and major compressions of the magnetosphere. Such compressions could well enhance plasma transport down the magnetotail, either as large-scale plasmoids (as first proposed by Vasyliūnas, 1983) or as small-scale "drizzle" (Kivelson & Southwood, 2005).…”

Section: Density Mapsmentioning

confidence: 76%

Survey of Juno Observations in Jupiter's Plasma Disk: Density

et al. 2021

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We explore the variation in plasma conditions through the middle magnetosphere of Jupiter with latitude and radial distance using Juno‐JADE measurements of plasma density (electrons, protons, sulfur, and oxygen ions) surveyed on Orbits 5–26 between March 2017 and April 2020. On most orbits, the densities exhibit regular behavior, mapping out a disk between 10 and 50 RJ (Jovian radii). In the disk, the heavy ions are confined close to the centrifugal equator which oscillates relative to the spacecraft due to the ∼10° tilt of Jupiter's magnetic dipole. Exploring each crossing of the plasma disk shows there are some occasions where the density profiles are smooth and well‐defined. At other times, small‐scale structures suggest temporal and/or spatial variabilities. There are some exceptional orbits where the outer regions (30–50 RJ) of the plasma disk show uniform depletion, perhaps due to enhanced ejection of plasmoids down the magnetotail, possibly triggered by solar wind compression events.

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Section: Density Mapsmentioning

confidence: 76%

Survey of Juno Observations in Jupiter's Plasma Disk: Density

et al. 2021

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“…The magnetopause is the region where the source of the magnetic field changes: inside the magnetopause, the controlling magnetic field is that of Jupiter; while outside, it is the solar wind magnetic field.The magnetosheath is the interface of the solar wind-magnetosphere interaction, affecting the physical processes occurring within Jupiter's magnetopause. The magnetosheath magnetic field and plasma interact at the magnetopause and, consequently, with Jupiter's magnetosphere (Ranquist et al, 2020). Therefore, studying the properties of turbulence in the magnetosheath helps to better understand the dynamical coupling between the solar wind and the magnetosphere and to improve the current models.…”

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confidence: 99%

Observation of Kolmogorov Turbulence in the Jovian Magnetosheath From JADE Data

Bandyopadhyay

McComas

Szalay

et al. 2021

Geophysical Research Letters

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The solar wind is the supersonic outward flow of plasma from the Sun. When the turbulent solar wind approaches Jupiter, it crosses a bow shock, which slows the plasma to subsonic speeds and causes significant increase in the plasma's density, temperature, and turbulence level. This region of subsonic plasma between the bow shock and magnetosphere is known as the magnetosheath. Magnetosheath of different sizes with varying properties is seen in the magnetospheres of Earth, Saturn, and Jupiter (Bagenal et al., 2017). The bounding surface of the magnetosphere is called the magnetopause. The magnetopause is the region where the source of the magnetic field changes: inside the magnetopause, the controlling magnetic field is that of Jupiter; while outside, it is the solar wind magnetic field.The magnetosheath is the interface of the solar wind-magnetosphere interaction, affecting the physical processes occurring within Jupiter's magnetopause. The magnetosheath magnetic field and plasma interact at the magnetopause and, consequently, with Jupiter's magnetosphere (Ranquist et al., 2020). Therefore, studying the properties of turbulence in the magnetosheath helps to better understand the dynamical coupling between the solar wind and the magnetosphere and to improve the current models. In addition, the interest in exploring plasma turbulence near Jupiter also lies in its plasma conditions: it has a strong magnetic field, a broad range of plasma β (the ratio of thermal pressure to magnetic pressure) values (Ranquist et al., 2019), and a very large system size, the combination makes the Jovian magnetospheric system a

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“…Figure 3c shows a TOF spectra from 2020-027 to 2020-028 when Juno was deep in the magnetotail at 110 RJ, −21° Jovian latitude, and midnight local time. This event is well inside all models for the magnetopause, where Figure 3d shows the 10%, 50%, and 90% boundaries (Joy et al, 2002;Ranquist et al, 2020). This example was chosen since it was one of the farthest magnetotail locations Juno reached at similar local times to the dispersive events.…”

Section: Open Vs Closed Magnetospheric Configurationmentioning

confidence: 75%

“…During this time, magnetospheric heavy ions (O n+ , S n+ ) are observed above ∼5 keV, exhibiting significant similarities to the composition of the magnetotail. Panel (d) shows the magnetosphere in the noon‐midnight plane, with the locations of (a) and (c) and three ranges of magnetopause boundaries (Ranquist et al., 2020 ).…”

Section: Open Vs Closed Magnetospheric Configurationmentioning

confidence: 99%

Closed Fluxtubes and Dispersive Proton Conics at Jupiter's Polar Cap

Szalay

Clark

Livadiotis

et al. 2022

Geophysical Research Letters

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The polar regions of Jupiter's magnetosphere are unlike those of any other planet explored by spacecraft with an internal magnetic field. Mercury (e.g., Anderson et al., 2010), Earth (e.g., Smith & Lockwood, 1996), and Saturn (e.g., Jasinski et al., 2014 all exhibit open magnetic topologies in their polar-most regions, where the solar wind is magnetically connected to each of these planets. Evidence for this solar wind connectivity has been found in magnetic field signatures associated with magnetopause transits (e.g., Gurnett et al., 2010) and direct observation of solar wind plasma composition and polar rain -field aligned solar wind strahl electrons that stream along the interconnected magnetic field toward the planet (Winningham & Heikkila, 1974).Jupiter's magnetosphere is internally driven by its strong, rapidly rotating magnetic field and Io's immense heavy ion plasma source. It likely has a fundamentally different magnetospheric interaction with the solar wind than the aforementioned planets ). Jupiter's intense auroral features are primarily driven by plasma processes throughout the magnetosphere and are an important diagnostic in understanding these complex processes (Delamere & Bagenal, 2010). These auroral features (e.g., Grodent, 2016) are typically categorized into: the oval-shaped main auroral emission, Galilean satellite footprint aurora, diffuse emissions equatorward of the main oval, and polar cap emissions poleward of the main oval (Figure 1). Polar cap emissions can exhibit rapid variations (e.g., Bonfond et al., 2016) and the mechanisms sustaining these emissions remain a mystery (e.g., Ebert et al., 2019). As the most poleward auroral features would map to the farthest distances from Jupiter, these auroral emissions have been used to diagnose Jupiter's solar wind interaction. Polar cap emissions have previously been interpreted to infer the presence of a Jovian cusp (Bunce et al., 2004). In contrast, a subsequent analysis interpreted these emissions to indicate a highly complex topological setup where the large majority of

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Polar Flattening of Jupiter's Magnetosphere

Cited by 4 publications

References 24 publications

Survey of Juno Observations in Jupiter's Plasma Disk: Density

Survey of Juno Observations in Jupiter's Plasma Disk: Density

Observation of Kolmogorov Turbulence in the Jovian Magnetosheath From JADE Data

Closed Fluxtubes and Dispersive Proton Conics at Jupiter's Polar Cap

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