Waves at the electron plasma frequency associated with solar wind magnetic holes: STEREO/Cluster observations

Briand, C.; Souček, J; Henri, Pierre; Mangeney, A.

doi:10.1029/2010ja015849

Cited by 21 publications

(27 citation statements)

References 52 publications

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“…Through a multispacecraft analysis using Helios 1 and 2 and Voyager 2 spacecraft data, Sperveslage et al (2000) 10.1029/2019JA027198 investigated the heliocentric radial dependence of MH occurrence rate between 0.3 and 17 AU. Other studies at 1 AU have reported ∼39% of all MHs are of linear type (Briand et al, 2010;Stevens & Kasper, 2007), while over the solar poles, nearly half of the magnetic depressions are linear MHs (Fränz et al, 2000;Tsurutani et al, 2011). Out of 850 MHs in the Sperveslage et al (2000) study, nearly 30% were linear holes, a rate much higher than the 13% rate observed in Ulysses data in the ecliptic plane (Tsurutani et al, 2009).…”

Section: Introductionmentioning

confidence: 57%

Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

et al. 2020

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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. Plain Language SummaryThe solar wind, a supersonic flow of electrons and ions flowing radially outward from the Sun, carries a magnetic field. Magnetic holes are structures with reduced magnetic field strength that last between a few seconds to a few minutes. These structures have been observed at many places throughout the solar system. A common formation mechanism for magnetic holes is a wave mode instability that converts magnetic energy into ion thermal energy, known as the mirror mode. Mirror mode instabilities grow when the temperature of ions moving perpendicular to the magnetic field is higher than that of ions moving in the parallel direction. Mirror waves alter the magnetic field and the spatial structure of the plasma. In this paper, we use observations from the Mars Atmosphere and Volatile EvolutioN spacecraft to study magnetic holes in the space environment around Mars.

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Section: Introductionmentioning

confidence: 57%

Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

et al. 2020

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“…While reported some Langmuir waves at individual discontinuities (25%), most Langmuir waves reported (75%) were associated with depressions in the overall magnetic field strength bounded by a pair of discontinuities, often called magnetic holes. Beam instabilities are thought to be excited at magnetic holes due to a combination of adiabatic motion and timeof-flight effects acting on strahl electrons as they traverse the bounding discontinuities Briand et al, 2010]. However, few of the CSs with nearby ESWs identified in the current study are positively identified as magnetic holes.…”

Section: Discussionmentioning

confidence: 73%

Electrostatic Solitary Waves in the Solar Wind: Evidence for Instability at Solar Wind Current Sheets

et al. 2013

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A strong spatial association between bipolar electrostatic solitary waves (ESWs) and magnetic current sheets (CSs) in the solar wind is reported here for the first time. This association requires that the plasma instabilities (e.g., Buneman, electron two stream) which generate ESWs are preferentially localized to solar wind CSs. Distributions of CS properties (including shear angle, thickness, solar wind speed, and vector magnetic field change) are examined for differences between CSs associated with ESWs and randomly chosen CSs. Possible mechanisms for producing ESW‐generating instabilities at solar wind CSs are considered, including magnetic reconnection.

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“…In a recent study Briand et al (2010) have shown that the polarization of the waves is compatible with Langmuir/z-mode waves. Through combined observations of STEREO and CLUSTER they have also demonstrated that the presence of a pronounced electron strahl is required for the generation of Langmuir waves and that the electron distribution function inside the magnetic hole is more isotropic compare to outside the hole.…”

Section: Langmuir Waves: From Linear To Nonlinear Plasma Physicsmentioning

confidence: 89%

Commission 49: Interplanetary Plasma and Heliosphere

Gopalswamy¹,

Mann²,

Bougeret³

et al. 2011

Proc. IAU

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Commission 49 (Interplanetary Plasma and Heliosphere) is part of IAU Division II (Sun and Heliosphere). The research topics include large-scale solar disturbances such as coronal mass ejections (CMEs), shocks, and corotating interaction regions (CIRs) propagating into the heliosphere. The disturbances propagate through the solar wind, which essentially defines the heliosphere. The solar disturbances provide large-scale laboratory to study plasma processes over various time and spatial scales, the highest spatial scale being the size of the heliosphere itself (~100 AU). These solar disturbances are related to solar activity in the form of active regions and coronal holes. Solar eruptions are accompanied by particle acceleration and the particles can be hazardous to life on earth in various ways from modifying the ionosphere to damaging space technology and increasing lifetime radiation dosage to astronauts and airplane crew. Particle acceleration in solar eruptions poses fundamental physics questions because the underlying mechanisms are not fully understood. One of important processes is the particle acceleration by shocks, which occurs throughout the heliosphere. The heliosphere has both neutral and ionized material, with interesting interaction between the two components.

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Waves at the electron plasma frequency associated with solar wind magnetic holes: STEREO/Cluster observations

Cited by 21 publications

References 52 publications

Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

Magnetic Holes Upstream of the Martian Bow Shock: MAVEN Observations

Electrostatic Solitary Waves in the Solar Wind: Evidence for Instability at Solar Wind Current Sheets

Commission 49: Interplanetary Plasma and Heliosphere

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