Storm-time Signatures of High-Latitude Convection on Subauroral and Low-latitude Ionosphere

Details Storm-time Signatures of High-Latitude Convection on Subauroral and Low-latitude Ionosphere Storm-time Signatures of High-Latitude Convection on Subauroral and Low-latitude Ionosphere

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsa14a..03s&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SA14A-03

Physics

[2411] Ionosphere / Electric Fields, [2431] Ionosphere / Ionosphere/Magnetosphere Interactions, [2435] Ionosphere / Ionospheric Disturbances, [2788] Magnetospheric Physics / Magnetic Storms And Substorms

Scientific paper

It is well known that during geomagnetically disturbed times, signatures of high-latitude enhanced convection can be observed in the ionosphere equatorward of the auroral oval with many types of ground-based or low-earth-orbit spaceborne instruments that either directly measure or infer electric fields or ion drifts. At low latitudes, the most commonly observed signature of enhanced convection is prompt-penetration electric fields. In the sub-auroral region, fast regions of westward convection narrowly confined in latitude are often observed in the dusk to midnight MLT sector within the main ionospheric trough, which are often termed Subauroral Ion drift events (SAIDs), polarization jets, or subauroral polarization streams (SAPS). Multi-instrument observations for strong magnetic storms of the last solar maximum supplied a wealth of information on penetration electric fields and SAPS phenomena. We use the Rice Convection Model (RCM) to present a physical picture of the SAPS and penetration electric fields in the context of ionosphere-magnetosphere coupling. By presenting simulation results for several large magnetic storms and comparing them with observations, we explain the basic physics behind the SAPS and penetration electric field phenomena, as well as discuss the areas where the model is not able to explain observations.

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