Energetic phenomena on the Sun that evoke significant geospace response over a timescale of minutes to days are mass emissions (CMEs and high speed streams) and electromagnetic transients (solar flares). CMEs and flares originate from closed magnetic field regions, while high speed streams originate from open field regions on the Sun. CMEs are responsible for large solar energetic particle events and major geomagnetic storms. High speed streams form CIRs, which can also lead to moderate geomagnetic storms. Flares can modify the conductivity of the ionosphere. The conditions created by the energetic phenomena are collectively termed space weather, which has emerged as an important natural hazard to life and society in various ways. Predicting the occurrence of these energetic phenomena and how the geospace responds to them has become an important task for the solar terrestrial science community. Once a closed field region appears on the Sun, when will it erupt? When it will not erupt? Will it produce only confined flares or it will involve mass ejections? How do CMEs develop shocks that accelerate SEPs? When and with what magnetic structure do CMEs arrive at Earth? How do CMEs propagate to Earth and what substructures cause geomagnetic disturbances? After a coronal hole appears on the solar disk, when will the associated CIR and high speed stream arrive at Earth and with what speeds? These are some of the questions that are being addressed in developing prediction schemes using various techniques. This session invited papers that discuss any of these issues that will contribute to the improvement in predicting the energetic phenomena and their geospace response.