Solar Wind Electron Proton Alpha Monitor (SWEPAM) for the Advanced Composition Explorer

McComas, D. J.; Bame, S. J.; Barker, P. F.; Feldman, W. C.; Phillips, J. L.; Riley, Pete; Griffee, J. W.

doi:10.1007/978-94-011-4762-0_20

Cited by 616 publications

(631 citation statements)

References 34 publications

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“…The 1 min resolution solar wind ion data detected by the instrument of Solar Wind Electron, Proton, and Alpha Monitor [McComas et al, 1998] and 16 s resolution magnetic field data acquired by the magnetic field detected instrument of MAG [Smith et al, 1998] on the ACE satellite are collected from the years of 1998 to 2005.…”

Section: Data Descriptionmentioning

confidence: 99%

X lines in the magnetotail for southward and northward IMF conditions

et al. 2015

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Utilizing associated observations of Geotail and ACE satellites from the year of 1998 to 2005, we investigated the X lines in the near‐Earth tail under different interplanetary magnetic field (IMF) conditions. The X lines are recognized by the tailward fast flows with negative Bz. Statistically, the X lines in the tail can be observed for southward as well as northward IMF, but more frequently observed for southward IMF. A typical case on 26 April 2005 showed clear evidence that the X line can occur for northward IMF while the geomagnetic activity is particularly quiet. Further analysis showed that the X line‐related solar wind has stronger Ey and Bz components for southward than northward IMF. In addition, the X line‐related geomagnetic activities are stronger for southward than northward IMF.

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Section: Data Descriptionmentioning

confidence: 99%

X lines in the magnetotail for southward and northward IMF conditions

et al. 2015

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“…Figure 2 shows data from the mag- netic field (MAG) and solar wind (SWEPAM) instruments (Smith et al, 1998;McComas et al, 1998); the data have been time-shifted to the bowshock using a minimum variance analysis technique based upon the work of Weimer et al (2003). The top two panels (a-b) display the IMF B Y and B Z components respectively; B Y was predominantly westward throughout the day except for an hour after midnight and B Z was mostly negative (southward), moving gradually northward as the day progressed.…”

Section: Overviewmentioning

confidence: 99%

Energetic electron precipitation during sawtooth injections

Kavanagh

Donovan

et al. 2007

Ann. Geophys.

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Abstract. We present simultaneous riometer observations of cosmic noise absorption in the nightside and dawn-noon sectors during sawtooth particle injections during 18 April 2002. Energetic electron precipitation (>30 keV) is a feature of magnetospheric substorms and cosmic radio noise absorption acts as a proxy for qualitatively measuring this precipitation. This event provides an opportunity to compare the absorption that accompanies periodic electron injections with the accepted paradigm of substorm-related absorption. We consider whether the absorption is consistent with the premise that these injections are quasi-periodic substorms and study the effects of sustained activity on the level of precipitation. Four consecutive electron injection events have been identified from the LANL (Los Alamos National Laboratory) geosynchronous data; the first two showing that additional activity can occur within the 2-4 h sawtooth periodicity. The first three events have accompanying absorption on the nightside that demonstrate good agreement with the expected pattern of substorm-absorption: discrete spike events with poleward motion at the onset followed by equatorward moving structures and more diffuse absorption, correlated with optical observations. Dayside absorption is linked to gradient-curvature drifting electrons observed at geostationary orbit and it is shown that low fluxes can lead to a lack of absorption as precipitation is suppressed; precipitation begins when the drifting electron flux surpasses some critical level following continuous injections of electrons from the magnetotail. In addition it is shown that the apparent motion of absorption determined from an azimuthal chain of riometers exhibits an acceleration that may be indicative of an energisation of the drifting electron population.

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“…For the November 8 -11 CME, we also present in-ecliptic plasma observations made by the Genesis ion monitor [Barraclough et al, 2003], the ACE electron spectrometer [McComas et al, 1998] and magnetometer [Smith et al, 1998]. Shocks were identified in the data as simultaneous discontinuous transitions in the speed, density, temperature, and magnetic field.…”

Section: Cme Observationsmentioning

confidence: 99%

Properties of high‐latitude CME‐driven disturbances during Ulysses second northern polar passage

Reisenfeld

Gosling

Forsyth

et al. 2003

Geophysical Research Letters

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[1] Ulysses observed five coronal mass ejections (CMEs) and their associated disturbances while the spacecraft was immersed in the polar coronal hole (CH) flow above 70°N in late 2001. Of these CMEs, two were very fast (>850 km s À1 ) driving strong shocks in the wind ahead, and two others were over-expanding. The two fast CMEs were observed leaving the Sun by LASCO/SOHO, and were observed in the ecliptic by Genesis and ACE. These were large events, spanning at least from the northern heliospheric pole to the ecliptic. Onedimensional hydrodynamic simulations indicate that these could be described as overpressured CMEs launched from the Sun at speeds initially faster than ambient, but then decelerating to the ambient solar wind speed as they propagated outward. The two over-expanding CMEs mark their first occurrence since Ulysses' first orbit when such CMEs were only observed in polar CH flow.

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Solar Wind Electron Proton Alpha Monitor (SWEPAM) for the Advanced Composition Explorer

Cited by 616 publications

References 34 publications

X lines in the magnetotail for southward and northward IMF conditions

X lines in the magnetotail for southward and northward IMF conditions

Energetic electron precipitation during sawtooth injections

Properties of high‐latitude CME‐driven disturbances during Ulysses second northern polar passage

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