The magnetopause energetic electron layer, 1. Observations along the distant magnetotail

Baker, D. N.; Stone, E. C.

doi:10.1029/ja083ia09p04327

Cited by 47 publications

(16 citation statements)

References 13 publications

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“…1) the outbound pass through the magnetosheath in late October 1983 at -100 Re downtail, we estimate from close examination of the data that the last electron burst was detected a distance of -5-6 Re from the last magnetopause crossing. These observations are consistent with previous reports of a "layer" of streaming energetic electrons extending 1-5 Re outside the magnetopause and observed to at least 40-60 Re downtail (Meng and Anderson, 1975;Baker and Stone, 1978). Our observations suggest that this layer extends to at least 200 Re down the tail, albeit with a considerably reduced electron intensity (Fig.…”

Section: Electron Bursts In the Magnetosheathsupporting

confidence: 83%

Energetic (>0.2 MeV) Electron Bursts in the Deep Geomagnetic Tail Observed by ISEE 3: Association with Substorms and Magnetotail Structures

Richardson

Owen

Slavin

1996

J. geomagn. geoelec

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Brief 0.2-2 MeV electron bursts were detected in the plasma sheet, tail lobes and magnetosheath by the Goddard Space Flight Center Medium Energy Cosmic Ray Experiment during the ISEE 3 geotail mission in 1982-3. We summarize the main features of these data and their implications for the structure and dynamics of the geomagnetic tail. Sharp falls in the intensity and occurrence rate of plasma sheet events at -90 Re from Earth suggest a change from predominantly closed field lines Earthward of this location to predominantly open field lines at greater distances downtail. The electron anisotropies and associated plasma flows support this proposal which is also consistent with other ISEE 3 observations suggesting that the tail neutral line typically lies at around this distance. Electron bursts in the tail are closely association with substorm activity onsets as indicated by AL intensifications and particle injections at geosynchronous orbit. Signatures of plasmoid ejection down the tail may be observed following electron bursts. In the deep tail, energetic electron enhancements tend to be observed close to the time of substorm onset and are not generally present in the plasma sheet and plasma sheet boundary layer at other times. This suggests that the electrons are accelerated at the substorm neutral line rather than along the current sheet, and are lost rapidly from the tail along open field lines.

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Section: Electron Bursts In the Magnetosheathsupporting

confidence: 83%

Energetic (>0.2 MeV) Electron Bursts in the Deep Geomagnetic Tail Observed by ISEE 3: Association with Substorms and Magnetotail Structures

Richardson

Owen

Slavin

1996

J. geomagn. geoelec

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“…The pitch angle distribution of 41-52 keV electrons during an electron burst is shown in Fig. 1g and h. The magnetic field components during this time period indicate these particles are streaming tailward, consistent with previous observations further downtail along the magnetopause (Baker and Stone, 1978). Energetic ions enhancements were also observed during this period and are shown in Fig.…”

Section: C2 Measurementssupporting

confidence: 72%

“…2). Monitoring energetic electrons (E > 200 keV) along the magnetopause further downtail (−10 R E < X SM < −40 R E ), Baker and Stone (1978) found a similar power law tail with γ ranging from 2 to 4 with a standard value of 3. This is consistent with the observations presented here and made just poleward of the cusp.…”

Section: C2 Measurementsmentioning

confidence: 90%

“…At high latitudes poleward of the cusp, Domingo et al (1977) observed energetic electrons during more than 90 % of the passes of a two year study with the HEOS-2 spacecraft. Further downtail Baker and Stone (1978) found energetic (E > 200 keV) electrons present during 97 % of the boundary passes by the IMP-8 spacecraft. Additional properties of the electron population at high latitudes include a positive correlation with geomagnetic indices (Meng and Anderson, 1975;Baker and Stone, 1977), a peak in intensity near the cusp (Formisano and Domingo, 1979), and a continual tailward flow (Baker and Stone, 1978).…”

Section: Introductionmentioning

confidence: 99%

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Energetic electrons along the high-latitude magnetopause

et al. 2012

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Abstract.A case study is presented to determine the source of the energetic electron layer frequently observed along the high-latitude magnetopause. Measurements by the Cluster spacecraft show bursts of field-aligned electrons occurring during time periods with high potential for dayside reconnection. These properties are compared with the expected signatures from several sources including escape from the exterior cusp, acceleration in a reconnection region, and release from the dayside trapping region through reconnection. The observed properties are most consistent with the electrons being released from the magnetosphere due to reconnection. In this model the electrons would flow along the newly reconnected IMF draped along the magnetopause and propagate along the high-latitude magnetopause. These observations demonstrate an active source for populating the energetic particle layer frequently observed along and just outside the high-latitude magnetopause.

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“…They occur especially in the Earth's magnetotail in the anti-Sun direction, but also in the magnetosheath which extends to ±∼30 • from the anti-Sun direction, and around the bow shock (to ±∼45 • from anti-Sun); see, e.g., Sarris et al (1976), Baker & Stone (1978), Meng et al (1981). They arise during geomagnetic activity.…”

Section: A2 Particle Event or Not?mentioning

confidence: 99%

Restless quiescence: thermonuclear flashes between transient X-ray outbursts

Kuulkers¹,

Zand

Lasota

2009

A&A

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For thermonuclear flashes to occur on neutron-star surfaces, fuel must have been accreted from a donor star. However, sometimes flashes are seen from transient binary systems when they are thought to be in their quiescent phase, during which no accretion, or relatively little, is expected to occur. We investigate the accretion luminosity during several such flashes, including the first-ever and brightest detected flash from Cen X-4 in 1969. We infer from observations and theory that immediately prior to these flashes the accretion rate must have been between about 0.001 and 0.01 times the equivalent of the Eddington limit, which is roughly 2 orders of magnitude less than the peak accretion rates seen in these transients during an X-ray outburst and 3-4 orders of magnitude more than the lowest measured values in quiescence. Furthermore, three such flashes, including the one from Cen X-4, occurred within 2 to 7 days followed by an X-ray outburst. A long-term episode of enhanced, but low-level, accretion is predicted near the end of the quiescent phase by the disk-instability model, and may thus have provided the right conditions for these flashes to occur. We discuss the possibility of whether these flashes acted as triggers of the outbursts, signifying a dramatic increase in the accretion rate. Although it is difficult to rule out, we find it unlikely that the irradiance by these flashes is sufficient to change the state of the accretion disk in such a dramatic way.

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The magnetopause energetic electron layer, 1. Observations along the distant magnetotail

Cited by 47 publications

References 13 publications

Energetic (>0.2 MeV) Electron Bursts in the Deep Geomagnetic Tail Observed by ISEE 3: Association with Substorms and Magnetotail Structures

Energetic (>0.2 MeV) Electron Bursts in the Deep Geomagnetic Tail Observed by ISEE 3: Association with Substorms and Magnetotail Structures

Energetic electrons along the high-latitude magnetopause

Restless quiescence: thermonuclear flashes between transient X-ray outbursts

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