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Chiu, M.C.; Von-Mehlem, U.I.; Willey, Cliff E.; Betenbaugh, Theresa; Maynard, J.J.; Krein, J.A.; Conde, R.F.; Gray, W.T.; Hunt, J.W.; Mosher, Larry; McCullough, M.G.; Panneton, Paul E.; Staiger, J.P.; Rodberg, Elliot H.

doi:10.1023/a:1005002013459

Cited by 53 publications

(29 citation statements)

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“…A stream of fast solar wind (∼700 km s −1 ) then led to a geomagnetic storm which began to develop at 01:30 UT on 22 January 2004 (strong B z >0 of ∼20 nT). Near the L1 point in the solar wind upstream of the Earth, between 00:00 UT and 10:00 UT, the ACE spacecraft (Chiu et al, 1998), showed interplanetary magnetic field conditions typical of lobe reconnection configurations, with B z mostly positive and strong B y <0, which lasted for the entire period considered here. According to ACE, the CME reached the spacecraft around 01:00 UT, when the solar wind velocity jumped from 450 to nearly 700 km s −1 .…”

Section: General Descriptionmentioning

confidence: 81%

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

Simon¹,

Lilensten²,

Moen

et al. 2007

Ann. Geophys.

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Abstract. We present for the first time a numerical kinetic/fluid code for the ionosphere coupling proton and electron effects. It solves the fluid transport equations up to the eighth moment, and the kinetic equations for suprathermal particles. Its new feature is that for the latter, both electrons and protons are taken into account, while the preceding codes (TRANSCAR) only considered electrons. Thus it is now possible to compute in a single run the electron and ion densities due to proton precipitation. This code is successfully applied to a multi-instrumental data set recorded on 22 January 2004. We make use of measurements from the following set of instruments: the Defence Meteorological Satellite Program (DMSP) F-13 measures the precipitating particle fluxes, the EISCAT Svalbard Radar (ESR) measures the ionospheric parameters, the thermospheric oxygen lines are measured by an all-sky camera and the H α line is given by an Ebert-Fastie spectrometer located at Ny-Ålesund. We show that the code computes the H α spectral line profile with an excellent agreement with observations, providing some complementary information on the physical state of the atmosphere. We also show the relative effects of protons and electrons as to the electron densities. Computed electron densities are finally compared to the direct ESR measurements.

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Section: General Descriptionmentioning

confidence: 81%

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

Simon¹,

Lilensten²,

Moen

et al. 2007

Ann. Geophys.

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show abstract

“…The EISCAT Svalbard Radar (ESR) is located at Longyearbyen (78. The Interplanetary magnetic field (IMF) and plasma parameters of the solar wind were obtained from the ACE spacecraft (Chiu et al, 1998) located near the L1 point. In this paper we have used data from the magnetic field experiment (MAG; Smith et al, 1998) and solar wind velocity data from the Solar Wind Electron Proton Alpha Monitor (SWEPAM; McComas, 1998) to estimate the time delay between ACE and the magnetopause.…”

Section: Instrumentationmentioning

confidence: 99%

On the diurnal variability in F2-region plasma density above the EISCAT Svalbard radar

Moen

Carlson³

et al. 2008

Ann. Geophys.

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Abstract. Two long runs of EISCAT Svalbard Radar (ESR), in February 2001 and October 2002, have been analysed with respect to variability in the F2 region peak density and altitude. The diurnal variation in the F2 peak density exhibits one maximum around 12:00 MLT and another around 23:00 MLT, consistent with solar wind controlled transport of EUV ionized plasma across the polar cap from day to night. High density plasma patch material is drawn in through the cusp inflow region independent of IMF B Y . There is no apparent IMF B Y asymmetry on the intake of high density plasma, but the trajectory of its motion is strongly B Y dependent. Comparison with the international reference ionosphere model (IRI2001) clearly demonstrates that the model does not take account of the cross-polar transport of F2-region plasma, and hence has limited applicability in polar cap regions.

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“…Solar wind parameters were obtained from the ACE spacecraft (Chiu et al, 1998) located near the L1 point in the solar wind upstream of the Earth. On 18 December 2001, the position of the spacecraft was (240, 27, 4) R E in GSM coordinates.…”

Section: Instrumentationmentioning

confidence: 99%

Multi-instrument mapping of the small-scale flow dynamics related to a cusp auroral transient

et al. 2005

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Abstract. In this paper we focus on flux transfer events (FTEs) and poleward moving auroral forms (PMAFs) in the cusp region, combining data from the EISCAT Svalbard radar, SuperDARN HF radars, ground-based optics, and three low-altitude polar-orbiting spacecraft. During an interval of southward interplanetary magnetic field the EISCAT Svalbard radar tracked a train of narrow flow channels drifting into the polar cap. One 30-60 km wide flow channel surrounded by flow running in the opposite direction is studied in great detail from when it formed equatorward of the cusp aurora, near magnetic noon, until it left the field-of-view and disappeared into the polar cap. Satellite data shows that the flow channel was on open field lines. The flow pattern is consistent with field-aligned currents on the sides of the flow channel; with a downward current on the equatorward side, and an upward current on the poleward side. The poleward edge of the flow channel was coincident with a PMAF that separated from the background cusp aurora and drifted into the polar cap. A passage of the DMSP F13 spacecraft confirms that the FTE flow channel was still discernable over 15 minutes after it formed, as the spacecraft revealed a 30-40 km wide region of sunward flow within the anti-sunward background convection. From the dimensions of the flow channel we estimate that the magnetic flux contained in the event was at least 1 MWb. This data set also shows that Birkeland current filaments often seen by low-altitude spacecraft in the cusp/mantle are really associated with individual FTE events or a train of FTEs in progress. As the region 0 or cusp/mantle current represents the statistical average consistent with the large-scale flow pattern, we therefore introduce a new term -FTE currents -to denote the unique pair of Birkeland current sheets that are associated with individual meso-scale FTE flow disturbances. The poleward movingCorrespondence to: K. Oksavik (kjellmar.oksavik@jhuapl.edu) auroral forms (PMAFs), often referred to in the literature, are the optical signature of the upward FTE current.

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Cited by 53 publications

References 0 publications

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

On the diurnal variability in F2-region plasma density above the EISCAT Svalbard radar

Multi-instrument mapping of the small-scale flow dynamics related to a cusp auroral transient

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