We present a community-led assessment of the solar system investigations achievable with NASA's next-generation space telescope, the Wide Field InfraRed Survey Telescope (WFIRST). WFIRST will provide imaging, spectroscopic, and coronagraphic capabilities from 0.43-2.0 µm and will be a potential contemporary and eventual successor to JWST. Surveys of irregular satellites and minor bodies are where WFIRST will excel with its 0.28 deg 2 field of view Wide Field Instrument (WFI). Potential ground-breaking discoveries from WFIRST could include detection of the first minor bodies orbiting in the Inner Oort Cloud, identification of additional Earth Trojan asteroids, and the discovery and characterization of asteroid binary systems similar to Ida/Dactyl. Additional investigations into asteroids, giant planet satellites, Trojan asteroids, * Corresponding authors: B.J. Holler (bholler@stsci.edu) and S.N. Milam (stefanie.n.milam@nasa.gov). Earth, similar to the James Webb Space Telescope [2]. (Spacecraft images from wfirst.gsfc.nasa.gov) Figure 2: The WFI field of view covers 0.28 deg 2 and is composed of 18 separate 4k´4k HgCdTe detectors. The fields of view for the Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3) instruments on HST and the Near-Infrared Camera (NIRCam) instrument on JWST are shown for comparison [2].WFIRST will operate at the Earth-Sun L2 point and its primary goal will be to carry out the following science programs: (1) an exoplanet microlensing survey near the galactic bulge, (2) CGI observations of exoplanets, (3) imaging and grism spectroscopy of galaxies at high galactic latitude, (4) a supernova survey with 3 different imaging depths and a spectroscopy component, and (5) Guest Observer (GO) science. Funding for the analysis of survey data outside the defined science teams will be part of the Guest Investigator (GI) program. GO programs are expected to comprise ~1.5 years, or approximately 25%, of the nominal mission duration.The imaging and spectroscopic capabilities of WFIRST [1,2] are well-suited for studies of solar system objects. In particular, the wavelength ranges of the IFC (0.6-2.0 µm) and the WFI (0.43-2.0 µm) cover diagnostic absorption features due to atmospheric gases, as well as minerals and ices on the surfaces of terrestrial bodies. The IFC provides spectral information over its entire