Effects of the interplanetary magnetic field y component on the dayside aurora

Abstract

Abstract A dawn–dusk asymmetry in many high-latitude ionospheric and magnetospheric phenomena, including the aurora, can be linked to the east–west (y) component of the interplanetary magnetic field (IMF). Owing to the scarcity of observations in the Southern Hemisphere, most of the previous findings are associated with the Northern Hemisphere. It has long been suspected that if the IMF B y component also produces a dawn–dusk asymmetry and/or a mirror image in the Southern Hemisphere as predicted by some theories. The present study explores the effect of the IMF B y component on the dayside aurora from both hemispheres by analyzing the auroral emission data from the Global UltraViolet scanning spectrograph Imager on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics mission spacecraft from 2002 to 2007. The data set comprises 28,774 partial images of the northern hemispheric oval and 29,742 partial images of the southern hemispheric oval, allowing for a statistical analysis. It is found that even though auroras in different regions of the dayside oval respond differently to the orientation of the IMF B y component, their responses are opposite between the two hemispheres. For example, at ~ 1400–1600 MLT in the Northern Hemisphere, where the so-called 1500 MLT auroral hot spots occur, peak auroral energy flux is larger for negative IMF B y comparing to positive IMF B y . The response is reversed in the Southern Hemisphere. The present study also suggests that the total energy flux does not change with the IMF B y orientation change. This result is consistent with a larger (smaller) convection vortex in the postnoon sector for IMF B y 0) resulting from anti-parallel merging.

Keywords

• Dayside aurora
• Hemispheric asymmetry
• TIMED
• GUVI
• FUV