Authors: S. Raptis (Johns Hopkins Applied Physics Laboratory), D. L. Turner (Johns Hopkins Applied Physics Laboratory), T. Horbury (Imperial College London), D. Chakrabarty (PRL-Gujarat, India), E. Christian (NASA Goddard Space Flight Center), C. M. S. Cohen (California Institute of Technology), M. E. Cuesta (Princeton University), M. A. Dayeh (Southwest Research Institute), R. Ebert (Southwest Research Institute), H. A. Farooki (Princeton University), M. Gkioulidou (Johns Hopkins Applied Physics Laboratory), C. O. Lee (Space Sciences Laboratory, University of California – Berkeley), Connor O’ Brien (Johns Hopkins Applied Physics Laboratory), S. Pal (IIT Roorkee), J. S. Rankin (Princeton University), K. Sankarsubramanian (URSC, India), A. Szabo (NASA Goddard Space Flight Center), R. Torbert (University of New Hampshire), D. Vassiliadis (NOAA/NESDIS/SWO), S. Vines (Southwest Research Institute), L. B. Wilson III (NASA Goddard Space Flight Center), and D. J. McComas (Princeton University).

For decades, ACE, Wind, and DSCOVR provided steady and valuable measurements of solar wind from the L1 point. However, multi-scale investigation of solar wind was limited due to the number of satellites at the L1 point. The arrival of Aditya-L1, and more recently of IMAP, and SOLAR-1 has fundamentally changed this landscape, forming a multiscale constellation. This fleet offers new capabilities to study the solar wind, especially the physical processes that drive particles from thermal populations into suprathermal and energetic ranges.

The discussion will help us examine how these missions could provide insight on several fundamental physical processes that we were unable to do so before. By synthesizing data across the fleet, we can track the evolution of turbulence, resolve shock dynamics, understand the coherence or lack of multiscale processes, and quantify the energization of particles. Furthermore, we will discuss how this multi-point perspective allows us to map the mesoscale structure of the solar wind and understand the large-scale transients that drive geo-effectiveness. Ultimately, the question we want to understand is how to use this new L1 fleet to move from localized observations to a system-wide understanding of how the solar wind evolves spatially and temporally.