SpringerImages - A statistical comparison of three ionospheric proxies for the OCB (see text for full details). The radial co-ordinate represents the difference in AACGM latitude between each proxy and the DMSP proxy, and the azimuthal co-ordinate represents MLT with magnetic local noon at the top of the figure. The DMSP proxy is shown in yellow at 0° latitude difference. For the other proxies the mean latitude difference in each 1-h MLT bin is shown by a coloured square and the standard deviations by the radial error bars. The Polar UVI proxy is shown in red and a red dashed line shows a low-order harmonic expansion fit to the mean latitude differences (from Carbary et al. 2003). The SWB proxy is shown in blue in the 1900–2400 MLT sector (from Chisham et al. 2004) and the 0000–1200 MLT sector (from Chisham et al. 2005a). The SWB proxy above 74° latitude in the 1200–1900 MLT sector is shown in green (from Chisham et al. 2005c)

A statistical comparison of three ionospheric proxies for the OCB (see text for full details). The radial co-ordinate represents the difference in AACGM latitude between each proxy and the DMSP proxy, and the azimuthal co-ordinate represents MLT with magnetic local noon at the top of the figure. The DMSP proxy is shown in yellow at 0° latitude difference. For the other proxies the mean latitude difference in each 1-h MLT bin is shown by a coloured square and the standard deviations by the radial error bars. The Polar UVI proxy is shown in red and a red dashed line shows a low-order harmonic expansion fit to the mean latitude differences (from Carbary et al. 2003). The SWB proxy is shown in blue in the 1900–2400 MLT sector (from Chisham et al. 2004) and the 0000–1200 MLT sector (from Chisham et al. 2005a). The SWB proxy above 74° latitude in the 1200–1900 MLT sector is shown in green (from Chisham et al. 2005c)

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Fig 12

A statistical comparison of three ionospheric proxies for the OCB (see text for full details). The radial co-ordinate represents the difference in AACGM latitude between each proxy and the DMSP proxy, and the azimuthal co-ordinate represents MLT with magnetic local noon at the top of the figure. The DMSP proxy is shown in yellow at 0° latitude difference. For the other proxies the mean latitude difference in each 1-h MLT bin is shown by a coloured square and the standard deviations by the radial error bars. The Polar UVI proxy is shown in red and a red dashed line shows a low-order harmonic expansion fit to the mean latitude differences (from Carbary et al. 2003). The SWB proxy is shown in blue in the 1900–2400 MLT sector (from Chisham et al. 2004) and the 0000–1200 MLT sector (from Chisham et al. 2005a). The SWB proxy above 74° latitude in the 1200–1900 MLT sector is shown in green (from Chisham et al. 2005c)

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Figure 12 summarizes the results of Chisham et al.

This is illustrated in Fig. 12 where the red symbols represent the mean latitudinal offsets determined by Carbary et al.

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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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