SpringerImages - An estimate of the global distribution of field-aligned currents in the northern hemisphere ionosphere at 2228–2230 UT on April 10, 1997, determined using SuperDARN and Polar UVI data. The colour indicates the magnitude and direction of the current, the blue represents upward current and the red/yellow represents downward current (see colour bar for scale). The black solid contour lines represent contours of Pedersen conductance determined from a combination of the Polar UVI data and a model of photoionization. The projection of the prevailing IMF vector on the Y-Z GSM plane is shown in the bottom-right corner. This figure is adapted from Bristow and Lummerzheim (2001)

An estimate of the global distribution of field-aligned currents in the northern hemisphere ionosphere at 2228–2230 UT on April 10, 1997, determined using SuperDARN and Polar UVI data. The colour indicates the magnitude and direction of the current, the blue represents upward current and the red/yellow represents downward current (see colour bar for scale). The black solid contour lines represent contours of Pedersen conductance determined from a combination of the Polar UVI data and a model of photoionization. The projection of the prevailing IMF vector on the Y-Z GSM plane is shown in the bottom-right corner. This figure is adapted from Bristow and Lummerzheim (2001)

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Fig 9

An estimate of the global distribution of field-aligned currents in the northern hemisphere ionosphere at 2228–2230 UT on April 10, 1997, determined using SuperDARN and Polar UVI data. The colour indicates the magnitude and direction of the current, the blue represents upward current and the red/yellow represents downward current (see colour bar for scale). The black solid contour lines represent contours of Pedersen conductance determined from a combination of the Polar UVI data and a model of photoionization. The projection of the prevailing IMF vector on the Y-Z GSM plane is shown in the bottom-right corner. This figure is adapted from Bristow and Lummerzheim (2001)

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Figure 9 shows an example of the FACs determined from the SuperDARN convection maps and Polar UVI images for a 2-min interval on April 7, 1997.

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A decade of the Super Dual Auroral Radar Network (SuperDARN): scientific achievements, new techniques and future directions

by Chisham, G.; Lester, M.; Milan, S. E.; Freeman, M. P.; Bristow, W. A.; Grocott, A.; McWilliams, K. A.; Ruohoniemi, J. M.; Yeoman, T. K.; Dyson, P. L.; Greenwald, R. A.; Kikuchi, T.; Pinnock, M.; Rash, J. P. S.; Sato, N.; Sofko, G. J.; Villain, J.-P.; Walker, A. D. M.
Journal: Surveys in Geophysics Vol. 28 Issue 1
DOI: 10.1007/s10712-007-9017-8
Published: 2007-06-07
Institution(s): Natural Environment Research Council, University of Leicester, UAF Geophysical Institute, University of Saskatchewan, Johns Hopkins University, La Trobe University, Nagoya University, University of KwaZulu-Natal, National Institute of Polar Research, LPCE/CNRS

Abstract

The Super Dual Auroral Radar Network (SuperDARN) has been operating as an international co-operative organization for over 10 years. The network has now grown so that the fields of view of its 18 radars cover the majority of the northern and southern hemisphere polar ionospheres. SuperDARN has been successful in addressing a wide range of scientific questions concerning processes in the magnetosphere, ionosphere, thermosphere, and mesosphere, as well as general plasma physics questions. We commence this paper with a historical introduction to SuperDARN. Following this, we review the science performed by SuperDARN over the last 10 years covering the areas of ionospheric convection, field-aligned currents, magnetic reconnection, substorms, MHD waves, the neutral atmosphere, and E-region ionospheric irregularities. In addition, we provide an up-to-date description of the current network, as well as the analysis techniques available for use with the data from the radars. We conclude the paper with a discussion of the future of SuperDARN, its expansion, and new science opportunities.

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	SuperDARN
	Magnetosphere
	Ionosphere
	HF radar
	Ionospheric convection
	Magnetic reconnection
	Substorms
	Magnetic field-aligned currents
	ULF waves
	Gravity waves
	Mesospheric winds
	Ionospheric irregularities

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