The Induced Magnetospheres of Mars, Venus, and Titan

Bertucci, C.; Duru, F.; Edberg, Niklas J. T.; Fräenz, M.; Martinecz, C.; Szegö, K.; Вайсберг, О. Л.

doi:10.1007/978-1-4614-3290-6_5

Cited by 41 publications

(53 citation statements)

References 172 publications

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“…It has a much wider opening angle (45°), indicating that the bow shock is supported by the tension force of the magnetic field lines which are draped around the obstacle by the flow, and cannot escape into the downstream region. Similar draping effects are detected around planets, moons, solar coronal mass ejections, and galaxies [46][47][48][49][50].…”

Section: MMsupporting

confidence: 60%

“…Over time this growing two-fluid separation is expected to produce an electric field, which in turn decelerates the flow of ions causing the transition into a shock front separate from the main stagnation shock [ figure 4(d)]. It is noted that these experimental observations are pertinent in the context of space physics as they provide support for a fast-flow braking mechanism previously postulated to occur in auroral magnetospheric events [43,45], and also bear some similarity to solar wind interactions with planetary ionospheres, which act as obstacles with highly conducting boundaries, leading to induced magnetospheres around planets and moons which do not possess magnetic cores [46,47].…”

Section: MMmentioning

confidence: 61%

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Interactions of magnetized plasma flows in pulsed-power driven experiments

Suttle

Burdiak

Cheung

et al. 2019

Plasma Phys. Control. Fusion

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A supersonic flow of magnetized plasma is produced by the application of a 1 MA-peak, 500 ns current pulse to a cylindrical arrangement of parallel wires, known as an inverse wire array. The plasma flow is produced by the × acceleration of the ablated wire material, and a magnetic field of several Tesla is embedded at source by the driving current. This setup has been used for a variety of experiments investigating the interactions of magnetized plasma flows. In experiments designed to investigate magnetic reconnection, the collision of counter-streaming flows, carrying oppositely directed magnetic fields, leads to the formation of a reconnection layer in which we observe ions reaching temperatures much greater than predicted by classical heating mechanisms. The breakup of this layer under the plasmoid instability is dependent on the properties of the inflowing plasma, which can be controlled by the choice of the wire array material. In other experiments, magnetized shocks were formed by placing obstacles in the path of the magnetized plasma flow. The pile-up of magnetic flux in front of a conducting obstacle produces a magnetic precursor acting on upstream electrons at the distance of the ion inertial length. This precursor subsequently develops into a steep density transition via ion-electron fluid decoupling. Obstacles which possess a strong private magnetic field affect the upstream flow over a much greater distance, providing an extended bow shock structure.In the region surrounding the obstacle the magnetic pressure holds off the flow, forming a void of plasma material, analogous to the magnetopause around planetary bodies with self-generated magnetic fields.

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Section: MMsupporting

confidence: 60%

Section: MMmentioning

confidence: 61%

Interactions of magnetized plasma flows in pulsed-power driven experiments

Suttle

Burdiak

Cheung

et al. 2019

Plasma Phys. Control. Fusion

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“…Following the nomenclature of a Geophysical Research Letters 10.1029/2020GL089230 similar structure at active comets (Neubauer, 1987) the layer where the magnetic field strength gradient occurs received the name magnetic pileup boundary (MPB) (Acuña et al, 1998). Pre-MAVEN measurements (Bertucci et al, 2011;Dubinin et al, 2008) have shown that the MPB is located between the region dominated by the solar plasma-the magnetosheath-and that governed by the plasma of planetary origin-the magnetic pileup region (MPR), also called induced magnetosphere-which is characterized by a strong and organized magnetic field of solar origin as a result of pileup and draping (Bertucci et al, 2003). Once again these features apply for regions where crustal fields are not important.…”

Section: Introductionmentioning

confidence: 99%

The Magnetic Structure of the Subsolar MPB Current Layer From MAVEN Observations: Implications for the Hall Electric Force

Boscoboinik

Bertucci

Gomez

et al. 2020

Geophysical Research Letters

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We report on the local structure of the Martian subsolar magnetic pileup boundary (MPB) from minimum variance analysis of the magnetic field measured by the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft for six orbits. In particular, we detect a well-defined current layer within the MPB and provide a local estimate of its current density which results in a sunward Hall electric force. This force accounts for the deflection of the solar wind ions and the acceleration of electrons which carry the interplanetary magnetic field through the MPB into the magnetic pileup region. We find that the thickness of the MPB current layer is of the order of both the upstream (magnetosheath) solar wind proton inertial length and convective gyroradius. This study provides a high-resolution view of one of the components of the current system around Mars reported in recent works. Plain Language Summary We investigate the current layer associated with the outer boundary of the Martian induced magnetosphere in the subsolar sector from selected MAVEN magnetic field and solar wind plasma observations. We measure the variance of the magnetic field across the boundary to obtain its normal, which in turn is used to measure the strength of the current density. The current density we obtain is such that its derived Hall electric force is strong enough to stop the solar wind ions at the outer boundary of Mars magnetosphere. On the other hand, this force would push the solar wind electrons and the interplanetary magnetic field frozen into the electron plasma into the induced magnetosphere. We also find that the thickness of this current layer in terms of typical lengths of the solar wind ion plasma is similar to the thickness of the terrestrial magnetopause.

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“…The relatively weak gravitational potential of Mars means that, in particular, atmospheric atomic and molecular hydrogen is observed in significant abundances out to many tens of Martian radii, forming what is known as the hydrogen exosphere (Anderson & Hord, 1971;Anderson, 1974;Chaufray et al, 2008;Chaffin et al, 2015). Mars is an unmagnetized planet, and the lack of a dipole magnetic field results in an induced magnetosphere with a bow shock located close to and upstream of the planet, at a distance of about 1.5 Mars radii from the center of the planet (Bertucci et al, 2011;Brain et al, 2003;Slavin et al, 1991;Vignes et al, 2000). These conditions mean that the neutral hydrogen exosphere extends upstream far beyond the planetary bow shock and is exposed to the flowing solar wind.…”

Section: Introductionmentioning

confidence: 99%

The Modulation of Solar Wind Hydrogen Deposition in the Martian Atmosphere by Foreshock Phenomena

et al. 2019

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The neutral exosphere of Mars extends far upstream beyond the bow shock, and as a result, solar wind protons can charge exchange with this neutral exosphere to produce energetic neutral atoms. Energetic neutral atoms produced directly upstream of Mars will precipitate into the Martian dayside atmosphere, where some fraction can undergo a charge stripping reaction and can be observed as “penetrating protons.” Clear, quasiperiodic modulations in penetrating proton densities are observed during certain Mars Atmosphere and Volatile EvolutioN (MAVEN) periapsis passes, and we show that these modulations occur during radial interplanetary magnetic field conditions. During such times, the region sunward of Mars is defined by quasi‐parallel shock conditions, generating foreshock structures characterized by enhancements in magnetic field strength, enhancements in proton density, and deceleration and deflection of the solar wind flow. These structures are observed at time cadences equal to the modulation of penetrating proton densities at periapsis. Particle tracing simulations show that the convection of these structures with the solar wind leads to localized enhancements in the rate of charge exchange upstream of the shock, producing the observed temporal variations in penetrating proton densities at periapsis. The observation of modulated penetrating proton densities at periapsis can thus be used to infer the existence of radial interplanetary magnetic field conditions upstream of the bow shock at Mars at times when MAVEN does not sample the upstream solar wind.

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The Induced Magnetospheres of Mars, Venus, and Titan

Cited by 41 publications

References 172 publications

Interactions of magnetized plasma flows in pulsed-power driven experiments

Interactions of magnetized plasma flows in pulsed-power driven experiments

The Magnetic Structure of the Subsolar MPB Current Layer From MAVEN Observations: Implications for the Hall Electric Force

The Modulation of Solar Wind Hydrogen Deposition in the Martian Atmosphere by Foreshock Phenomena

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