Electromagnetic cyclotron waves (ecws) are extensively observed in the solar wind from 0.3 to 1 AU. They appear to be left-hand or right-hand polarized in the spacecraft frame and propagate in…

The Smithsonian Institution, operating through its Smithsonian Astrophysical Observatory (SAO) in Cambridge, Massachusetts, was awarded a $91,621 research grant on January 29, 2020, with completion scheduled for January 28, 2025. The grant supports scientific investigation into electromagnetic cyclotron waves observed in the solar wind between 0.3 and 1 astronomical unit from the sun, with particular focus on understanding the interaction between solar wind ions and electromagnetic waves through new observational data and hybrid simulation modeling. The research addresses fundamental questions about wave polarization, propagation characteristics, and ion dynamics, including temperature anisotropy and relative drifts among ion populations such as proton cores, proton beams, and alpha particles in non-equilibrium solar wind conditions. This award carries no set-aside designation and was funded through a civilian federal agency.

As a premier research institution specializing in space science and astrophysical disciplines, SAO brings substantial expertise in heliophysics and solar physics to this investigation. The organization has an established track record of delivering sophisticated scientific research and technical support across diverse space science missions, with extensive prior federal contract awards from NASA's Science Mission Directorate and the National Science Foundation. This grant aligns with SAO's core competencies in particle physics, plasma dynamics, and data analysis systems that support advancing understanding of solar wind phenomena critical to space weather prediction and heliospheric science.

Electromagnetic cyclotron waves (ecws) are extensively observed in the solar wind from 0.3 to 1 AU. They appear to be left-hand or right-hand polarized in the spacecraft frame and propagate in directions close to the background magnetic field. On the other hand, the solar wind is often not in equilibrium, featured with the temperature anisotropy of particles with respect to the background magnetic field and relative drifts among ION components (proton core, proton beam, and alpha particles).