Session P3 - Multi-techniques to monitor the Sun and solar wind for space weather

Stephan G. Heinemann (Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany), Eleanna Asvestari (University of Helsinki, Helsinki, Finland), Camilla Scolini (Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, US)

Interplanetary coronal mass ejections, interplanetary shocks, stream and co-rotating interaction regions (SIRs/CIRs) and high speed solar wind streams are the primary drivers of strong to minor geomagnetic activity and play a major role in shaping the heliospheric environment in which they propagate. Therefore, understanding the heliospheric solar wind, ambient magnetic field, and their solar sources are vital in validating and refining space weather forecasting efforts. The aim of this session is to address the characteristics of these flows, the heliospheric background solar wind structure in which they propagate with respect to their solar source regions through the means of observations and models. Newly launched missions including Parker Solar Probe (PSP) and Solar Orbiter (SolO), as well as, established missions such as the Solar Dynamics Observatory (SDO) and the Solar Terrestrial Relations Observatories (STEREOs) provide a multitude of information that may be used to validate, improve, and refine current knowledge in this field. We encourage submissions relating to solar wind sources both for slow and fast wind, solar wind acceleration/ejection, interplanetary coronal mass ejections and shocks, stream interaction, and the structure of the magnetic field and plasma topology at the source surface and in the inner heliosphere. We advocate for authors to present their work that utilizes observations and/or models with relation to space weather.