SpringerImages - (a) The line-of-sight Doppler velocities measured by the northern hemisphere SuperDARN radars in the 1658–1700 UT interval on April 6, 2000. (b) The Map Potential ionospheric convection map for the same interval. Both maps are presented in a geomagnetic latitude–MLT coordinate system, with magnetic local midnight at the bottom, noon at the top, dawn to the right, and dusk to the left. The small coloured dots show the origin of the velocity vectors and the length and colour of the vectors indicate the magnitude of the flow (see colour table for scale). Flow vectors are only shown in regions where there was line-of-sight velocity input. The full equipotential solution is shown in (b) by the solid (afternoon convection cell) and dashed (morning convection cell) black lines. The dashed blue line (only visible in the dayside ionosphere) represents the Heppner–Maynard convection boundary which constrains the extent of the mapping. The letters at different MLTs mark the MLT locations of the radars that contributed data to the map (see Table , Fig. ). At the bottom right of panel (b) is shown the projection of the prevailing IMF (red arrow) onto the Y-Z GSM plane, and the maximum potential difference across the polar cap (ΦPC) determined from the mapping

(a) The line-of-sight Doppler velocities measured by the northern hemisphere SuperDARN radars in the 1658–1700 UT interval on April 6, 2000. (b) The Map Potential ionospheric convection map for the same interval. Both maps are presented in a geomagnetic latitude–MLT coordinate system, with magnetic local midnight at the bottom, noon at the top, dawn to the right, and dusk to the left. The small coloured dots show the origin of the velocity vectors and the length and colour of the vectors indicate the magnitude of the flow (see colour table for scale). Flow vectors are only shown in regions where there was line-of-sight velocity input. The full equipotential solution is shown in (b) by the solid (afternoon convection cell) and dashed (morning convection cell) black lines. The dashed blue line (only visible in the dayside ionosphere) represents the Heppner–Maynard convection boundary which constrains the extent of the mapping. The letters at different MLTs mark the MLT locations of the radars that contributed data to the map (see Table , Fig. ). At the bottom right of panel (b) is shown the projection of the prevailing IMF (red arrow) onto the Y-Z GSM plane, and the maximum potential difference across the polar cap (ΦPC) determined from the mapping

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Fig 2

(a) The line-of-sight Doppler velocities measured by the northern hemisphere SuperDARN radars in the 1658–1700 UT interval on April 6, 2000. (b) The Map Potential ionospheric convection map for the same interval. Both maps are presented in a geomagnetic latitude–MLT coordinate system, with magnetic local midnight at the bottom, noon at the top, dawn to the right, and dusk to the left. The small coloured dots show the origin of the velocity vectors and the length and colour of the vectors indicate the magnitude of the flow (see colour table for scale). Flow vectors are only shown in regions where there was line-of-sight velocity input. The full equipotential solution is shown in (b) by the solid (afternoon convection cell) and dashed (morning convection cell) black lines. The dashed blue line (only visible in the dayside ionosphere) represents the Heppner–Maynard convection boundary which constrains the extent of the mapping. The letters at different MLTs mark the MLT locations of the radars that contributed data to the map (see Table , Fig. ). At the bottom right of panel (b) is shown the projection of the prevailing IMF (red arrow) onto the Y-Z GSM plane, and the maximum potential difference across the polar cap (Φ_PC) determined from the mapping

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An example of these gridded line-of-sight velocity data, using data from 8 of the northern hemisphere SuperDARN radars, is shown in Fig. 2 a.

The result for an L = 8 fit, applied to the line-of-sight velocity data presented in Fig. 2 a, is shown in Fig. 2 b.

The line-of-sight velocity dataset used as input for the convection maps is often spatially extensive (as shown in Fig. 2 a), but not truly global.

In this case the IMF was measured by the ACE spacecraft with a time lag of 34 min, and its projection in the Y-Z GSM plane is shown in the bottom right of Fig. 2 b.

In Fig. 2 b the Heppner–Maynard boundary is depicted as a dashed blue line.

2 b.

The convection maps are presented in a similar format to Fig. 2 b.

The convection maps are presented in the same format as Fig. 2 b.

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

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