[P-EM09] Space Weather and Space Climate

[PEM09-P06] Analyzing the Effects of Coronal Hole Parameters and their Evolutions on High-Speed Solar Winds

*Chi-Shun Liao¹, Ya-Hui Yang¹ (1.Department of Space Science and Engineering, National Central University, Taiwan)

Keywords:coronal hole, solar wind, CIR

Coronal hole is a magnetically open region on solar disk, which appears as a dark area in solar extreme ultraviolet images due to its relatively low plasma density and temperature compared to ambient regions. The high-speed solar winds originated from the open magnetic field structures of a coronal hole would produce a stream interaction region (SIR) when the fast solar wind hits the slow solar wind ahead, leading to a geomagnetic storm potentially. To quantify the coronal hole parameters and determine their effects on the high-speed solar winds, the AIA 193 Å images, HMI line-of-sight magnetograms, and solar wind measurements at 1 AU during 2010-2021 are analyzed here by correlating the temporal variation profiles of plasma and magnetic field quantities studied. We also characterize the effects of coronal hole spatial distributions on the speeds of high-speed streams. In addition, the long-lived coronal holes causing the co-rotating interaction regions (CIRs) and recurrent geomagnetic disturbances are especially discussed to clarify the influence of coronal hole evolutions on high-speed solar winds.