Investigating the Effects of Coronal Holes on the Interplanetary Solar Wind Parameters

Solar emissions have a high impact on the Earth’s magnetic field, and the prediction of solar events is of high interest. Solar wind high-speed streams (HSSs) are considered the principal generator of geomagnetic activity during the declining phase of the solar cycle. These HSSs originated from solar coronal holes (CHs), which are observed by Euv observations of the solar surface. The HSSs are considered the main driver of CIR-driven storms. Although these storms are not considered severe storms, CIR-driven geomagnetic storms can cause recurrent geomagnetic storms that may last for several days and produce high fluxes of relativistic electrons. CH’s position and area on the solar surface are highly correlated to the solar wind (SW) speed at 1AU. Accurate solar wind speed forecasting is a vital aspect that provides a deeper understanding of solar variability and its corresponding effects on Earth. Various techniques have been used to predict the solar wind using mathematical models, MHD models, and Artificial neural network (ANN) models.

Here we aim to model the dependency of solar wind speed at 1 AU on the CH area. We used a homogeneous CH synoptic dataset through Carrington rotations: 1601 - 2185, covering May 1973 to January 2017, and HSS measurements at 1 AU to find their dependency using the machine learning (ML) network.