Motion of the dipolarization front during a flow burst event observed by Cluster

Nakamura, R.; Baumjohann, W.; Klecker, B.; Bogdanova, Y. V.; Balogh, A.; Rème, H.; Bosqued, J. M.; Dandouras, I.; Sauvaud, J. A.; Glaßmeier, K.‐H.; Kistler, L. M.; Mouikis, C.; Zhang, T. L.; Eichelberger, Hans; Runov, A.

doi:10.1029/2002gl015763

Cited by 375 publications

(397 citation statements)

References 13 publications

(18 reference statements)

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“…In the first event that we have chosen, 12 August 2001, there is a lot of dynamics going on in the current sheet. The data show a thinning current sheet (Nakamura et al, 2002a), sending the spacecraft to either side of it and a high wave power in the magnetic field. The second event on 29 August 2001 has the spacecraft move into the current sheet, but they do not cross B x = 0.…”

Section: Late Substorm Phase and Substorm Re-intensificationmentioning

confidence: 99%

Compressional waves in the Earth's neutral sheet

et al. 2004

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Abstract. Compressional waves in the Earth's current sheet, driven by the high-speed plasma flows connected to substorms, are investigated using the Cluster magnetometer and plasma instrument. During the time that Cluster had its apogee in the magnetotail (July through October 2001), we have studied 5 events in detail. We find compressional waves in the 30-60 mHz band, at a spectral power density that is dependent on when and where the event is observed. There is a difference of two orders of magnitude in power density between waves at substorm onset and waves during quiet times. Strong plasma flows are the driver of the wave power. The spacecraft location in the current sheet is also important for the spectral power density. Having four spacecraft available we can discern spatial from temporal variations. We have determined the propagation direction of the waves in the 30-60 mHz band and found that in the Cluster rest frame they propagate in the same direction as the plasma flow at an angle 30 • < φ < 40 • with respect to the plasma flow direction in the spacecraft' rest frame.

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Section: Late Substorm Phase and Substorm Re-intensificationmentioning

confidence: 99%

Compressional waves in the Earth's neutral sheet

et al. 2004

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“…Reconnection-Associated Phenomena in the Magnetotail In addition to diffusion region physics, of interest are kinetic physics in reconnection exhausts (bursty bulk flows), exhaust boundaries and separatrices, and reconnection jet fronts (also called "dipolarization fronts") (e.g., Nakamura et al 2002;Runov et al 2009) which may be important sites for particle energization . The planned MMS orbit is such that during the first science tail season (phase 1x), the apogee will be 12R E , with the apogee being raised to 25R E for the second science tail season (phase 2b) (Fuselier et al 2015, this issue).…”

Section: Magnetotailmentioning

confidence: 99%

Establishing the Context for Reconnection Diffusion Region Encounters and Strategies for the Capture and Transmission of Diffusion Region Burst Data by MMS

et al. 2015

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This paper describes the efforts of our Inter-Disciplinary Scientist (IDS) team to (a) establish the large-scale context for reconnection diffusion region encounters by MMS at the magnetopause and in the magnetotail, including the distinction between X-line and O-line encounters, that would help the identification of diffusion regions in spacecraft data, and (b) devise possible strategies that can be used by MMS to capture and transmit burst data associated with diffusion region candidates. At the magnetopause we suggest the strategy of transmitting burst data from all magnetopause crossings so that no magnetopause reconnection diffusion regions encountered by the spacecraft will be missed. The strategy is made possible by the MMS mass memory and downlink budget. In the magnetotail, it is estimated that MMS will be able to transmit burst data for all diffusion regions, all reconnection jet fronts (a.k.a. dipolarization fronts) and separatrix encounters, but less than 50 % of reconnection exhausts encountered by the spacecraft. We also discuss automated burst trigger schemes that could capture various reconnection-related phenomena. The identification of candidate diffusion region encounters by the burst trigger schemes will be verified and improved by a Scientist-In-The-Loop (SITL). With the knowledge of the properties of the region surrounding the diffusion region and the combination of automated burst triggers and further optimization by the SITL, MMS should be able to capture most diffusion regions it encounters.

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“…Spacecraft observations have shown that rapid enhancements in the B Z field represent spatial structures -dipolarization fronts (DFs) -which are typically observed at the leading edge of the earthwardmoving bursty bulk flows (BBFs) (e.g., Angelopoulos et al,742 A. Y. Malykhin et al: Contrasting dynamics of electrons and protons 1992; Nakamura et al, 2002;Runov et al, 2009). DFs are associated with electron and ion acceleration (e.g., Apatenkov et al, 2007;Asano et al, 2010;Zhou et al, 2010;Fu et al, 2011;Birn et al, 2011;Grigorenko et al, 2017) as well as with various wave activities, e.g., whistler emissions, lower hybrid and electron cyclotron waves (e.g., Le Contel et al, 2009;Zhou et al, 2009;Deng et al, 2010;Khotyaintsev et al, 2011;Hwang et al, 2011;Vilberg et al, 2014;Grigorenko et al, 2016).…”

Section: Introductionmentioning

confidence: 99%

“…It was shown that dipolarizations occur at different timescales and can be roughly classified into two groups: (i) the propagating isolated DFs observed during a few minutes (e.g., Nakamura et al, 2002;Runov et al, 2009;Fu et al, 2011;Schmid et al, 2011) and (ii) the socalled "secondary" dipolarizations related to the flow braking and flux pile up in the near-Earth tail (e.g., ). The secondary dipolarizations are observed during much longer time periods (up to several hours) and usually are associated with the formation of the substorm current wedge (SCW) (McPherron et al, 1973;Sergeev et al, 2012;Yao et al, 2012).…”

Section: Introductionmentioning

confidence: 99%

Contrasting dynamics of electrons and protons in the near-Earth plasma sheet during dipolarization

et al. 2018

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Abstract. The fortunate location of Cluster and the THEMIS P3 probe in the near-Earth plasma sheet (PS) (at X ∼ −7-−9 R E ) allowed for the multipoint analysis of properties and spectra of electron and proton injections. The injections were observed during dipolarization and substorm current wedge formation associated with braking of multiple bursty bulk flows (BBFs). In the course of dipolarization, a gradual growth of the B Z magnetic field lasted ∼ 13 min and it was comprised of several B Z pulses or dipolarization fronts (DFs) with duration ≤ 1 min. Multipoint observations have shown that the beginning of the increase in suprathermal (> 50 keV) electron fluxes -the injection boundary -was observed in the PS simultaneously with the dipolarization onset and it propagated dawnward along with the onset-related DF. The subsequent dynamics of the energetic electron flux was similar to the dynamics of the magnetic field during the dipolarization. Namely, a gradual linear growth of the electron flux occurred simultaneously with the gradual growth of the B Z field, and it was comprised of multiple short (∼ few minutes) electron injections associated with the B Z pulses. This behavior can be explained by the combined action of local betatron acceleration at the B Z pulses and subsequent gradient drifts of electrons in the flux pile up region through the numerous braking and diverting DFs. The nonadiabatic features occasionally observed in the electron spectra during the injections can be due to the electron interactions with high-frequency electromagnetic or electrostatic fluctuations transiently observed in the course of dipolarization.On the contrary, proton injections were detected only in the vicinity of the strongest B Z pulses. The front thickness of these pulses was less than a gyroradius of thermal protons that ensured the nonadiabatic acceleration of protons. Indeed, during the injections in the energy spectra of protons the pronounced bulge was clearly observed in a finite energy range ∼ 70-90 keV. This feature can be explained by the nonadiabatic resonant acceleration of protons by the bursts of the dawn-dusk electric field associated with the B Z pulses.

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Motion of the dipolarization front during a flow burst event observed by Cluster

Cited by 375 publications

References 13 publications

Compressional waves in the Earth's neutral sheet

Compressional waves in the Earth's neutral sheet

Establishing the Context for Reconnection Diffusion Region Encounters and Strategies for the Capture and Transmission of Diffusion Region Burst Data by MMS

Contrasting dynamics of electrons and protons in the near-Earth plasma sheet during dipolarization

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