Abstract
On May 23, 2000, proton auroras observed by IMAGE FUV on the dayside were very dynamic. Auroral pattern at the cusp footpoint is well correlated with IMF and solar wind parameters. A proton aurora brightened at high latitude poleward from the dayside oval after solar wind ion temperature increased while solar wind density and bulk speed were steady. It then vanished after IMF turned southward. Under this IMF condition, auroral activity occurred only in the dayside oval. As IMF Bz reverted to northward, cusp proton aurora reappeared at high latitude. The location of the cusp proton aurora changes with the IMF By polarity, consistent with previous reports. These results suggest an upstream source for the observed high‐latitude cusp proton aurora. One possible explanation is that bow shock energetic ions are transported into the cusp via the high‐latitude magnetic merging process to induce optical emissions in the ionosphere.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
