ARTEMIS Science Objectives

Sibeck, D. G.; Angelopoulos, V.; Brain, David; Delory, G. T.; Eastwood, J. P.; Farrell, W. M.; Grimm, R. E.; Halekas, J. S.; Hasegawa, Hiroshi; Hellinger, Petr; Khurana, K. K.; Lillis, Robert J.; Øieroset, M.; Phan, T. D.; Raeder, J.; Russell, C. T.; Schriver, D.; Slavin, J. A.; Trávníček, Pavel; Weygand, J. M.

doi:10.1007/s11214-011-9777-9

Cited by 51 publications

(34 citation statements)

References 202 publications

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“…In this event study, a burst of midtail BBFs was observed by the two ARTEMIS probes (Sibeck et al, ), P1 and P2, at ~05:25 UT on 6 December 2014 at X ~ −60 R E . ARTEMIS magnetic field vectors (3 s resolution) were measured by the fluxgate magnetometer (FGM) instrument (Auster et al, ), and plasma moments (3 s resolution) were measured by the electrostatic analyzer (ESA, 0.006–20 keV/q for ions and 0.007–26 keV for electrons) (McFadden et al, ) and the solid‐state telescope (SST, 35 keV–6 MeV for ions and 30 keV–6 MeV for electrons).…”

Section: Bbfs and Plasma Bubble In Midtailmentioning

confidence: 72%

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E

Wang

Xing²,

Liu

et al. 2018

JGR Space Physics

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We report the first observations that connect a burst of fast flows and Pi2 fluctuations in the midtail current sheet at X ~ −60 RE with ground magnetic negative bays and Pi2 pulsations at high latitudes near 70°. Both the flow burst and negative bays occurred around midnight and were isolated and lasted for ~10 min. The flow burst had the characteristics of a low‐density plasma bubble. It was moving earthward at ~340 km/s and was accompanied by field‐aligned currents. The timing and equatorward motion of magnetic bays can be accounted for by this earthward moving bubble. Enhanced Pi2 fluctuations were observed within both the bubble and the magnetic bays. Pressure anisotropy with higher parallel pressure was observed associated with the flow burst and was firehose unstable. We discuss firehose instability as one of the possible mechanisms for the Pi2 fluctuations.

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Section: Bbfs and Plasma Bubble In Midtailmentioning

confidence: 72%

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E

Wang

Xing²,

Liu

et al. 2018

JGR Space Physics

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“…THEMIS and ARTEMIS [ Angelopoulos , 2008, 2011; Sibeck et al , 2011] provide a new opportunity to examine global solar wind entry modes, by making simultaneous subsolar and distant flank observations for the first time. Here we present new observations from ARTEMIS showing the survival of FTE flux ropes far along the tail magnetopause at x = −67 R E on the dusk flank, with flux content similar to that of FTEs at the dayside.…”

Section: Introductionmentioning

confidence: 99%

Survival of flux transfer event (FTE) flux ropes far along the tail magnetopause

et al. 2012

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[1] During intervals of southward IMF, magnetic reconnection can result in the formation of flux transfer events (FTEs) on the dayside magnetopause which travel along the magnetopause in the anti-sunward direction. Of particular interest is their fate and the role they play transporting solar wind plasma into the magnetosphere. We present the discovery of FTEs far along the distant tail magnetopause (x = À67 Earth radii) using data from ARTEMIS on the dusk flank magnetopause under southward/duskward IMF conditions. The identification of several events is further supported by excellent fits to a force-free flux rope model. The axis of each structure is principally north-south, i.e., perpendicular to the Sun-Earth line. Simultaneous observations by THEMIS on the dayside magnetopause indicate that FTEs are being produced there, although perhaps 2-4 times smaller in size. The convection time from the dayside magnetopause to ARTEMIS is 30 min, and the FTEs have a flux content comparable to those typically observed on the dayside magnetopause, indicating that these features are in quasi-equilibrium as they are convected downtail. By considering the relative orientations of the FTEs observed by THEMIS and ARTEMIS, the magnetic field geometry is consistent with the FTEs being produced on the dayside magnetopause along an extended X-line in the presence of IMF B y and bending as they are convected to the flanks.

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“…The particle and magnetic field measurements from the two ARTEMIS probes (P1 and P2) [Sibeck et al, 2011] are used. The probes orbit the Moon with distances <~5 R E from the Moon.…”

Section: Datamentioning

confidence: 99%

Dawn‐dusk asymmetry in bursty hot electron enhancements in the midtail magnetosheath

et al. 2015

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Bursty (a few minutes) enhancements of hot electrons (1–10 keV) in the tail magnetosheath, which we name hot electron enhancements (HEEs), are sometimes observed. To understand the processes leading to HEEs, we have used 4 years of measurements from Acceleration Reconnection Turbulence and Electrodynamics of Moon's Interaction with the Sun mission to statistically investigate the dawn‐dusk asymmetry of HEEs in the midtail (x from −30 to −70 RE) magnetosheath and their correlations with the solar wind/interplanetary magnetic field (IMF) conditions. We find two strong dawn‐dusk asymmetries associated with HEEs: (1) they occur about 3 to 4 times more frequently on the dawnside. (2) Their fluxes on the dawnside are about twice as large as those on the duskside. The magnitudes of HEE fluxes are similar to those of the magnetosphere fluxes near the magnetopause, which are also a factor of 2 higher on the dawnside, indicating that the magnetosphere electrons are likely the source for HEEs and the cause for the HEE flux asymmetry. HEEs occur preferentially during higher solar wind speed, and the majority of HEEs are associated with sharp IMF direction changes and are accompanied by large and transient magnetosheath density changes. These correlations are stronger on the dawnside, suggesting that perturbations created near the quasi‐parallel bow shock, which is most of the time on the dawnside, associated with IMF discontinuities is a possible process leading to HEEs and could account for the higher HEE occurrence on the dawnside.

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ARTEMIS Science Objectives

Cited by 51 publications

References 202 publications

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E

Survival of flux transfer event (FTE) flux ropes far along the tail magnetopause

Dawn‐dusk asymmetry in bursty hot electron enhancements in the midtail magnetosheath

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ARTEMIS Science Objectives

Cited by 51 publications

References 202 publications

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 RE

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 RE

Survival of flux transfer event (FTE) flux ropes far along the tail magnetopause

Dawn‐dusk asymmetry in bursty hot electron enhancements in the midtail magnetosheath

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A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E

A Case Study of Connection Between Ground Magnetic Field Perturbations and Tail Current Sheet Bursty Flows at X = −60 R_E