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The Origin and Shape of Diffuse Auroral Patches Kyle Rae

The Origin and Shape of Diffuse Auroral Patches Kyle Rae E. Donovan, J. Liang, E. Spanswick, M. Lessard, S. Jones, and A. Jaynes. The Origin and Shape of Diffuse Auroral Patches Kyle Rae E. Donovan, J. Liang, E. Spanswick, M. Lessard, S. Jones, and A. Jaynes. Introduction: patchy aurora

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The Origin and Shape of Diffuse Auroral Patches Kyle Rae

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  1. The Origin and Shape of Diffuse Auroral Patches Kyle Rae E. Donovan, J. Liang, E. Spanswick, M. Lessard, S. Jones, and A. Jaynes

  2. The Origin and Shape of Diffuse Auroral Patches Kyle Rae E. Donovan, J. Liang, E. Spanswick, M. Lessard, S. Jones, and A. Jaynes Introduction: patchy aurora Motivation for what I am doing Method/Models Results

  3. 25 Minutes

  4. latitude 60 Minutes

  5. noon See also Jones et al., Large-scale aspects and temporal evolution of pulsating aurora, JGR, 2011.

  6. Nishimura, et al., Multievent study of the correlation between pulsating aurora and whistler mode chorus emissions, J. Geophys. Res., 2011; See also Jaynes et al., Poster, SM13B-2038.

  7. Map locus of points out to equatorial plane (T8

  8. Put particles of a given energy on that locus of points and let them move under EXB + grad B for some time… then trace that shape back onto the corresponding later image….

  9. Start 0 keV

  10. 6 minutes 0 keV 6 minutes 1 keV protons

  11. 6 minutes 0 keV and 0.5 keV protons

  12. Discussion We use the motion of patches and the evolution of their shape to learn something about the plasma in the magnetotail that (somehow) defines their shape. We identify a patch and trace part of its boundary to a model equatorial plane. We evolve that equatorial shape as though it was defined by particles of a given energy… we trace that shape back to the ionosphere and compare with an image of the aurora at the appropriate later time. Our results so far indicate that if the shape is determined in the magnetotail…. 1) The plasma that determines the shape has to be cold (<1 keV) 2) The plasma that determines the shape has to be low energy (<1 keV) We need to check how model dependent these results are (we think they are not). This work provides information relevant to the pitch angle scattering mechanism in the patchy aurora…. The shape of the patches is defined by a structure (depression or enhancement) in cold plasma density. This should be useful for probing inner magnetospheric convection.

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