IRTF Data Archive Program Information

# # Program information file # PROGRAM_ID 2021A038 PROGRAM_TITLE High Cadence Imaging of Io's Volcanos to Understand the Influence of the Jovian Magnetosphere and The Periodicity of Loki PROGRAM_INV1 Christian Tate PROGRAM_INV2 Julie Rathbun PROGRAM_INV3 Alexander Hayes PROGRAM_INV4 PROGRAM_INV5 PROGRAM_SCICAT solar system PROGRAM_ABSTRACT_BEG Io's volcanoes are constantly changing and influencing changes in the rest of the Jupiter system, including the Io torus and Jovian magnetosphere. Currently, the best way to understand Io's volcanic behavior is to use ground-based telescopes, and data from the IRTF has led to understanding volcanic eruptions at Loki and other locations [Rathbun et al., 2002; Rathbun and Spencer, 2006; Rathbun and Spencer, 2010]. Loki's period appears to have changed again recently, but more observations are necessary to determine the period. We request numerous short imaging observations of Io's near-IR volcanic thermal emission with SpeX and/or iSHELL in Jupiter eclipse, during Jupiter occultations, and in sunlight, to provide a high-time-resolution and record of volcanic activity during the Juno orbiter mission. This work has two goals: [1] To understand the influence of Io volcanism on the Jovian magnetosphere and aurorae being studied by Juno [as well as the Japanese Hisaki mission in Earth orbit]; and [2] To improve our understanding of the time variability of Io's volcanoes, in particular the remarkable periodic behavior of Loki, Io's largest volcano. Our observation strategy includes two types of observations: [1] 1.6 -- 4.8 um Jupiter eclipse imaging with 3.5-um Jupiter occultation imaging, providing spatially resolved mapping of temperatures, brightnesses, and locations of individual volcanoes on the Jupiter-facing hemisphere, in the absence of competition from reflected sunlight; and [2] 3.5 -- 4.8 micron sunlit imaging, providing lower spatial resolution mapping of the brightest volcanos at all Io longitudes [including the volcanos most likely to be large enough to affect the magnetosphere]. PROGRAM_ABSTRACT_END