The THEMIS Fluxgate Magnetometer

Auster, H. U.; Glaßmeier, Karl‐Heinz; Magnes, W.; Aydogar, Özer; Baumjohann, W.; Constantinescu, Dragoş; Fischer, D.; Fornaçon, K.‐H.; Georgescu, E.; Harvey, P.; Hillenmaier, O.; Kroth, R.; Ludlam, M.; Narita, Yasuhito; Nakamura, R.; Okrafka, K.; Plaschke, Ferdinand; Richter, Ingo; Schwarzl, H.; Stoll, B.; Valavanoglou, A.; Wiedemann, Martin

doi:10.1007/978-0-387-89820-9_11

Cited by 460 publications

(463 citation statements)

References 15 publications

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“…In this study we make use of 3 s time resolution plasma data obtained from the ESA (electrostatic analyzer; McFadden et al, 2008) instrument, while for the magnetic field data provided by the FGM (fluxgate magnetometer; Auster et al, 2008) instrument we make use of 0.25 and 3 s time resolutions.…”

Section: Analysis and Resultsmentioning

confidence: 99%

Dipolarization fronts in the near-Earth space and substorm dynamics

et al. 2015

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Abstract. During magnetospheric substorms and plasma transport in the Earth's magnetotail various magnetic structures can be detected. Dipolarization fronts and flux ropes are the most prominent structures characteristic for substorm dynamics. However, they are treated as separate magnetotail features independent of each other. In this paper, we analyze a number of dipolarization fronts observed by the THEMIS (Time History of Events and Macroscale Interactions during Substorms) spacecraft at different geocentric distances by applying the magnetohydrostatic Grad-Shafranov (GS) reconstruction technique. Our analysis shows that there is a possibility of dipolarization fronts to originate from highly dissipated flux ropes which are in the late stage of their evolution, subjected to a continuous magnetic deterioration due to the reconnection process. These results may improve our understanding of magnetoplasma processes in Earth's magnetotail.

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Section: Analysis and Resultsmentioning

confidence: 99%

Dipolarization fronts in the near-Earth space and substorm dynamics

et al. 2015

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“…At this time, ARTEMIS P1 sat just upstream from the Moon, in the undisturbed solar wind. We show a selection of the observations made by the electrostatic analyzer (ESA) [McFadden et al, 2008], fluxgate magnetometer (FGM) [Auster et al, 2008], electric field instrument (EFI) [Bonnell et al, 2008], and search-coil magnetometer (SCM) [Roux et al, 2008] instruments in Figure 1.…”

Section: High-altitude Observationsmentioning

confidence: 99%

Evidence for small‐scale collisionless shocks at the Moon from ARTEMIS

Halekas

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McFadden

et al. 2014

Geophysical Research Letters

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ARTEMIS observes structures near the Moon that display many properties commonly associated with collisionless shocks, including a discontinuity with downstream compression of magnetic field and density, heating and wave activity, and velocity deflections away from the Moon. The two-probe ARTEMIS measurements show that these features do not exist in the pristine solar wind and thus must result from lunar influences. Discontinuity analyses indicate mass flux and heating across the boundary, with the normal velocity dropping from supermagnetosonic to submagnetosonic across the discontinuity. The shock location with respect to crustal magnetic fields suggests a causal relationship, implying that solar wind protons reflected from crustal fields may produce the observed structures. These observations may indicate some of the smallest shocks in the solar system (in terms of plasma scales), driven by solar wind interaction with magnetic fields on the order of the ion gyroradius and inertial length.

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“…During fast survey mode, the spacecraft also returns ESA and SST particle distribution functions with reduced angular resolution every 3 s. We use the on-board computed moments, denoted as the "MOM" product, when showing the plasma velocity. The triaxial fluxgate magnetometer (FGM) measures the background magnetic field and its low frequency fluctuations up to 64 Hz [Auster et al, 2008]. …”

Section: Data Sets and Instrumentationmentioning

confidence: 99%

THEMIS observations of compressional poloidal pulsations in the dawnside magnetosphere: A case study

et al. 2013

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[1] We present results from a case study of compressional poloidal pulsations with periods ranging from 5 to 12 min in the dawn magnetosphere from 1630 to 2000 UT on 27 February 2011. However, we employ THEMIS (Time History of Events and Macroscale Interactions during Substorms) magnetic field, plasma, and energetic particle observations to determine azimuthal wavelengths (7000-27,000 km) and velocities (9-28 km/s) consistent with previous work. We then apply a new method invoking the north to south motion of the THEMIS spacecraft and the fact that the equatorial node exhibited north-south oscillations to derive the meridional structure of the wave in great detail. We determined that the amplitude of the meridional motion of the equatorial node was~0.8 R E , and that the meridional wave length exceeded 3 R E .

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The THEMIS Fluxgate Magnetometer

Cited by 460 publications

References 15 publications

Dipolarization fronts in the near-Earth space and substorm dynamics

Dipolarization fronts in the near-Earth space and substorm dynamics

Evidence for small‐scale collisionless shocks at the Moon from ARTEMIS

THEMIS observations of compressional poloidal pulsations in the dawnside magnetosphere: A case study

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