The Variation of Coronal Holes with Solar Cycle

Coronal holes are commonly known to be the source of the open magnetic flux and the high-speed solar wind. In EUV and X-ray emission lines, coronal holes are seen as the regions with reduced emission due to lower temperatures and electron density than the surrounding quiet sun. Observing the evolution of coronal holes over the course of a solar cycle, can lead to a greater understanding of the evolution of the solar dynamo and can advance our knowledge in forecasting space weather. Synoptic data from the Normal Incidence Spectrometer (NIS), which is part of the Coronal Diagnostic Spectrometer (CDS) onboard the Solar and Heliospheric Observatory (SoHO), have been used in this work to observe the evolution of coronal holes during cycle 23, from mid-1996 through to mid-2007 (solar minimum to solar minimum).

Autorentext

Graduated from University of Central Lancashire in 2001 with a Masters degree in Astrophysics. He continued his studies, gaining a PhD in Solar Astrophysics in 2008. He was then employed as the High Performance Computing Facility manager for the University, whilst maintaining an active role in NASA's Solar Dynamics Observatory project.