FGM Data Products in the CAA

Gloag, John; Lucek, E.; Alconcel, Leah-Nani; Balogh, A.; Brown, P.; Carr, C.; Dunford, Charlotte; Oddy, T.; Souček, J

doi:10.1007/978-90-481-3499-1_7

Cited by 23 publications

(17 citation statements)

References 3 publications

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“…This study makes use of data from a number of experiments on board the Cluster spacecraft, including PEACE (Johnstone et al, 1997;Fazakerley et al, 2010), the Fluxgate Magnetometer (FGM) (Balogh et al, 1997;Gloag et al, 2010), the Electric Field and Waves (EFW) experiment (Gustafsson et al, 1997;Khotyaintsev et al, 2010), the Waves of High frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) (Décréau et al, 1997;Trotignon et al, 2010), and the Spatio-Temporal Analysis of Field Fluctuations (STAFF) experiment (Cornilleau-Wehrlin et al, 1997.…”

Section: Datamentioning

confidence: 99%

Absence of the strahl during times of slow wind

Gurgiolo¹,

Goldstein

2017

Ann. Geophys.

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Abstract. It is not uncommon during periods when the solar wind speed is less than 425 km s −1 to observe near 1 AU no evidence of a strahl population in either the electron solar wind or within the foreshock. Estimating the fluid flow within each energy step returned from the Plasma Electron And Current Experiment (PEACE) on board Cluster-2 often finds that in slow wind the GSE spherical flow angles in energies above where there is a clear core/halo signature are often close to radial with no evidence of a field-aligned flow. This signifies the lack of a strahl presence in the electron velocity distribution function (eVDF). When there is no obvious strahl signature in the data, the electrons above the core/halo in energy appear to be unstructured and smeared in angle. This can either be interpreted as due to statistical noise in low counting rate situations or the result of intense scattering. Regions where the strahl is seen and not seen are often separated by a very thin boundary layer. These transitions in the spacecraft frame of reference can be quite rapid, generally occurring within one to two spins (4-8 s).

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Section: Datamentioning

confidence: 99%

Absence of the strahl during times of slow wind

Gurgiolo¹,

Goldstein

2017

Ann. Geophys.

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“…We used combined full-resolution data from the fluxgate magnetometer (FGM) (Balogh et al, 1997;Gloag et al, 2010) and together with waveform magnetic field data from Spatio-Temporal Analysis of Field Fluctuations (STAFF) (Cornilleau-Wehrlin et al, 1997 to produce magnetic field power spectra. Five vector per second FGM data are used to indicate the location of the projections of the magnetic field head and tail locations in all the phi-theta (φ-θ) plots used in the paper.…”

Section: Datamentioning

confidence: 99%

Observations of diffusion in the electron halo and strahl

Gurgiolo¹,

Goldstein

2016

Ann. Geophys.

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Abstract. Observations of the three-dimensional solar wind electron velocity distribution functions (VDF) using φ-θ plots often show a tongue of electrons that begins at the strahl and stretches toward a new population of electrons, termed the proto-halo, that exists near the projection of the magnetic field opposite that associated with the strahl. The energy range in which the tongue and proto-halo are observed forms a "diffusion zone". The tongue first appears in energy generally near the lower-energy range of the strahl and in the absence of any clear core/halo signature. While the φ-θ plots give the appearance that the tongue and proto-halo are derived from the strahl, a close examination of their density suggests that their source is probably the upper-energy core/halo electrons which have been scattered by one or more processes into these populations.

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“…Launched in 2000, the Cluster mission comprises 4 spacecraft, each with 11 instruments, investigating magnetic and electric fields, particle populations and waves. The instruments used in this study are the Fluxgate Magnetometer (FGM) [ Balogh et al , 2001; Gloag et al , 2010] and the CODIF (CIS) instruments [ Rème et al , 2001; Dandouras et al , 2010], both from the Cluster 3 spacecraft only. The data used are at spin resolution, obtained from the Cluster Active Archive (CAA) [ Perry et al , 2006; Laakso et al , 2010].…”

Section: Instrumentationmentioning

confidence: 99%

Storm and substorm effects on magnetotail current sheet motion

et al. 2012

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Passes through the mid‐region of the magnetotail by the Cluster spacecraft from 2001 to 2007 have been examined to study the dynamics of the cross‐tail current sheet. Cluster is ideally placed to study this region due to the orientation of the orbit in the magnetotail, such that the current sheet is sampled at distances downtail from about 8–19 RE. Multiple fluctuations of the X component of the magnetic field (BX) from positive to negative and vice versa, measured by Cluster as it crosses the nominal location of the current sheet, indicate that the current sheet is in motion. In this study we use the number of crossings of the current sheet by the Cluster 3 spacecraft as a measure of the dynamics of the magnetotail. The effects of substorm and magnetic storm activity on the dynamics during these orbits have been investigated using the AE and SYM‐H indices. Our results indicate that the current sheet is more often in motion during orbits when there is greater than average substorm activity and a quiet ring current. Results suggest that internal processes within the tail that initiate substorms may also initiate the flapping motion of the current sheet. In addition the more dipolar field that results from an enhanced ring current during magnetic storms may inhibit tail dynamics during substorm events.

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FGM Data Products in the CAA

Cited by 23 publications

References 3 publications

Absence of the strahl during times of slow wind

Absence of the strahl during times of slow wind

Observations of diffusion in the electron halo and strahl

Storm and substorm effects on magnetotail current sheet motion

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