Isolated magnetic field structures in Mercury's magnetosheath as possible analogues for terrestrial magnetosheath plasmoids and jets

Karlsson, Tomas; Liljeblad, Elisabet; Kullén, Anita; Raines, J. M.; Slavin, J. A.; Sundberg, T.

doi:10.1016/j.pss.2016.06.002

Cited by 38 publications

(48 citation statements)

References 58 publications

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“…Therefore, to increase our understanding of jets in different parameter ranges, we need to investigate plasma environments other than the Earth's magnetosheath. Karlsson et al (2016) have investigated whether structures analogous to magnetosheath jets or plasmoids exist in the Mercury magnetosheath. Due to limitations of the ion measurements on-board the MESSENGER spacecraft given the instrument placement and temporal resolution in the magnetosheath (Raines et al 2011), determination of flow velocity and density on small enough scales was not possible.…”

Section: Other Plasma Environmentsmentioning

confidence: 99%

“…Due to limitations of the ion measurements on-board the MESSENGER spacecraft given the instrument placement and temporal resolution in the magnetosheath (Raines et al 2011), determination of flow velocity and density on small enough scales was not possible. Instead Karlsson et al (2016) looked for isolated magnetic field structures similar to those associated with both diamagnetic and paramagnetic jets/plasmoids at Earth (see Sects. 4.2 and 5.2.2).…”

Section: Other Plasma Environmentsmentioning

confidence: 99%

“…For isolated magnetic field structures with a clear decrease in field strength ('negative structures') Karlsson et al (2016) concluded that these exist both in the pristine solar wind and in the magnetosheath (see Fig. 38), similar to Earth.…”

Section: Example System: Mercurymentioning

confidence: 99%

“…38). Karlsson et al (2016) concluded that these structures were likely FTEs. Since the magnetosheath end of an FTE flux rope should be associated with a lower plasma density than the surrounding magnetosheath, the positive magnetic field structures are not analogues to terrestrial paramagnetic plasmoids (but maybe the subset of terrestrial magnetosheath jets associated with FTEs, reported by ; see Sect.…”

Section: Example System: Mercurymentioning

confidence: 99%

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Jets Downstream of Collisionless Shocks

et al. 2018

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The magnetosheath flow may take the form of large amplitude, yet spatially localized, transient increases in dynamic pressure, known as "magnetosheath jets" or "plasmoids" among other denominations. Here, we describe the present state of knowledge with respect to such jets, which are a very common phenomenon downstream of the quasi-parallel bow shock. We discuss their properties as determined by satellite observations (based on both case and statistical studies), their occurrence, their relation to solar wind and foreshock conditions, and their interaction with and impact on the magnetosphere. As carriers of plasma and corresponding momentum, energy, and magnetic flux, jets bear some similarities to bursty bulk flows, which they are compared to. Based on our knowledge of jets in the near Earth environment, we discuss the expectations for jets occurring in other planetary and

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Section: Other Plasma Environmentsmentioning

confidence: 99%

Section: Other Plasma Environmentsmentioning

confidence: 99%

Section: Example System: Mercurymentioning

confidence: 99%

Section: Example System: Mercurymentioning

confidence: 99%

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Jets Downstream of Collisionless Shocks

et al. 2018

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“…In this study, unlike studies during the orbital phase of MESSENGER (e.g. Karlsson et al, 2016), there is no need to discuss the influence of solar activity, as can be seen in Fig. 2, top panel.…”

Section: Resultsmentioning

confidence: 99%

On the magnetic characteristics of magnetic holes in the solar wind between Mercury and Earth

Volwerk¹,

Goetz²,

Plaschke³

et al. 2019

Preprint

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Abstract. The occurrence rate of linear and pseudo magnetic holes has been determined during MESSENGER's cruise phase starting from Earth (2005) and arriving at Mercury (2011). It is shown that the occurrence rate of linear magnetic holes, defined as a maximum of 10° rotation of the magnetic field over the hole, slowly decreases from Mercury to Earth. The pseudo magnetic holes, defined as a rotation between 10° and 45° over the hole, have mostly a constant occurrence rate, with a slight increase in front of the Earth and a decrease around the Earth. The width and depth of these structures seem to strongly differ depending on whether they are inside or outside of Venus's orbit.

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Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

Madanian

Halekas

Mazelle

et al. 2019

Preprint

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Magnetic holes (MHs) are pressure‐balanced structures characterized by distinct decreases in the interplanetary magnetic field strength in otherwise unperturbed solar wind. In this paper we present an analysis of MHs upstream of the Martian bow shock based on 3 months of observations by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. Plasma properties within and around these structures as well as their shape characteristics are examined. We find an occurrence rate of around 2.1 events per day. About 51% of all events are of linear type with magnetic field rotation across the hole less than 10°. We observe linear MHs both as isolated events and as part of a train of MHs. The proton temperature anisotropy inside MHs increases, while alpha particles remain mostly isotropic. The average electron temperature inside MHs modestly increases with increasing hole depth. The duration of linear holes at 1.5 AU shows an increase compared to durations at smaller heliocentric distances, but the structures remain asymmetrical and ellipsoid. A case study of MHs accompanied by a population of heavy pickup ions is also discussed.

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Isolated magnetic field structures in Mercury's magnetosheath as possible analogues for terrestrial magnetosheath plasmoids and jets

Cited by 38 publications

References 58 publications

Jets Downstream of Collisionless Shocks

Jets Downstream of Collisionless Shocks

On the magnetic characteristics of magnetic holes in the solar wind between Mercury and Earth

Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

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