Observations of low‐frequency magnetic oscillations in the Martian magnetosheath, magnetic pileup region, and tail

Espley, J. R.; Cloutier, P. A.; Brain, David; Crider, D. H.; Acuña, M. H.

doi:10.1029/2003ja010193

Cited by 100 publications

(105 citation statements)

References 62 publications

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“…2). The slowed, shocked solar wind flows around the obstacle within the magnetosheath, a turbulent region (Espley et al 2004) bounded by the bow shock and a lower boundary, often referred to as the magnetic pile-up boundary (Bertucci et al 2003), or alternatively the induced magnetosphere boundary (e.g., Brain et al 2015) or induced magnetopause. It marks the narrow transition between plasma dominated by ions of solar wind origin and plasma dominated by ions of planetary origin; it is often approximated by a paraboloid of revolution about the planet-Sun line.…”

Section: Interaction With the Solar Windmentioning

confidence: 99%

The MAVEN Magnetic Field Investigation

et al. 2015

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The MAVEN magnetic field investigation is part of a comprehensive particles and fields subsystem that will measure the magnetic and electric fields and plasma environment of Mars and its interaction with the solar wind. The magnetic field instrumentation consists of two independent tri-axial fluxgate magnetometer sensors, remotely mounted at the outer extremity of the two solar arrays on small extensions ("boomlets"). The sensors are controlled by independent and functionally identical electronics assemblies that are integrated within the particles and fields subsystem and draw their power from redundant power supplies within that system. Each magnetometer measures the ambient vector magnetic field over a wide dynamic range (to 65,536 nT per axis) with a resolution of 0.008 nT in the most sensitive dynamic range and an accuracy of better than 0.05 %. Both magnetometers sample the ambient magnetic field at an intrinsic sample rate of 32 vector samples per second. Telemetry is transferred from each magnetometer to the particles and fields package once per second and subsequently passed to the spacecraft after some reformatting. The magnetic field data volume may be reduced by averaging and decimation, when necessary to meet telemetry allocations, and application of data compression, utilizing a lossless 8-bit differencing scheme. The MAVEN magnetic field experiment may be reconfigured in flight to meet unanticipated needs and is fully hardware redundant. A spacecraft magnetic control program was implemented to provide a magnetically clean environment for the magnetic sensors and the MAVEN mission plan provides for occasional spacecraft maneuversmultiple rotations about the spacecraft x and z axes-to characterize spacecraft fields and/or instrument offsets in flight.

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Section: Interaction With the Solar Windmentioning

confidence: 99%

The MAVEN Magnetic Field Investigation

et al. 2015

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“…The solar wind interaction regions of planets Venus and Mars are also prone to the generation of lowfrequency waves by pick-up ions (e.g. Luhmann et al, 1983;Espley et al, 2004). The terrestrial magnetosphere, however, is the classical environment to study ULF waves and eigenoscillations of an entire magnetosphere (e.g.…”

Section: Introductionmentioning

confidence: 99%

Quasiperiodic ULF-pulsations in Saturn's magnetosphere

et al. 2009

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Abstract. Recent magnetic field investigations made onboard the Cassini spacecraft in the magnetosphere of Saturn show the existence of a variety of ultra low frequency plasma waves. Their frequencies suggest that they are presumably not eigenoscillations of the entire magnetospheric system, but excitations confined to selected regions of the magnetosphere. While the main magnetic field of Saturn shows a distinct large scale modulation of approximately 2 nT with a periodicity close to Saturn's rotation period, these ULF pulsations are less obvious superimposed oscillations with an amplitude generally not larger than 3 nT and show a packagelike structure. We have analyzed these wave packages and found that they are correlated to a certain extent with the large scale modulation of the main magnetic field. The spatial localization of the ULF wave activity is represented with respect to local time and Kronographic coordinates. For this purpose we introduce a method to correct the Kronographic longitude with respect to a rotation period different from its IAU definition. The observed wave packages occur in all magnetospheric regions independent of local time, elevation, or radial distance. Independent of the longitude correction applied the wave packages do not occur in an accentuated Kronographic longitude range, which implies that the waves are not excited or confined in the same selected longitude ranges at all times or that their lifetime leads to a variable phase with respect to the longitudes where they have been exited.

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“…The term "low-frequency" is used here in the same sense as in Guicking et al (2010), Espley et al (2004), and Schwartz et al (1996): frequencies below or at the proton gyrofrequency. Great efforts have been undertaken to characterise and identify different wave modes (cf.…”

Section: Introductionmentioning

confidence: 99%

Low-frequency magnetic field fluctuations in Earth's plasma environment observed by THEMIS

et al. 2012

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Abstract. Low-frequency magnetic wave activity in Earth's plasma environment was determined based on a statistical analysis of THEMIS magnetic field data. We observe that the spatial distribution of low-frequency magnetic field fluctuations reveals highest values in the magnetosheath, but the observations differ qualitatively from observations at Venus presented in a previous study since significant wave activity at Earth is also observed in the nightside magnetosheath. Outside the magnetosheath the low-frequency wave activity level is generally very low. By means of an analytical streamline model for the magnetosheath plasma flow, we are able to investigate the spatial and temporal evolution of wave intensity along particular streamlines in order to characterise possible wave generation mechanisms. We observe a decay of wave intensity along the streamlines, but contrary to the situation at Venus, we obtain good qualitative agreement with the theoretical concept of freely evolving/decaying turbulence. Differences between the dawn region and the dusk region can be observed only further away from the magnetopause. We conclude that wave generation mechanisms may be primarily attributed to processes at or in the vicinity of the bow shock. The difference with the observations of the Venusian magnetosheath we interpret to be the result of the different types of solar wind interaction processes since the Earth possesses a global magnetic field while Venus does not, and therefore the observed magnetic wave activities may be caused by diverse magnetic field controlled characteristics of wave generation processes.

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Observations of low‐frequency magnetic oscillations in the Martian magnetosheath, magnetic pileup region, and tail

Cited by 100 publications

References 62 publications

The MAVEN Magnetic Field Investigation

The MAVEN Magnetic Field Investigation

Quasiperiodic ULF-pulsations in Saturn's magnetosphere

Low-frequency magnetic field fluctuations in Earth's plasma environment observed by THEMIS

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