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MINDS: Detection of an Inner Gas Disk Caused by Evaporating Bodies around HD 172555
M. Samland (Max Planck Institute for Astronomy), Thomas K. Henning (Max Planck Institute for Astronomy), A. Caratti o Garatti (Astronomical Observatory of Capodimonte, National Institute for Astrophysics), Teresa Giannini (Astronomical Observatory of Rome, National Institute for Astrophysics), Jeroen Bouwman (Max Planck Institute for Astronomy), Benoît Tabone (Centre National de la Recherche Scientifique, Université Paris-Saclay), Aditya M. Arabhavi (University of Groningen), Göran Olofsson (Stockholm University, AlbaNova), M. Güdel (University of Vienna, ETH Zurich), Nicole Pawellek (University of Vienna, Konkoly Observatory), I. Kamp (University of Groningen), L. B. F. M. Waters (Radboud University Nijmegen, Space Research Organisation Netherlands), Dmitry A. Semenov (Max Planck Institute for Astronomy), Ewine F. van Dishoeck (Leiden University, Max Planck Institute for Extraterrestrial Physics), Olivier Absil (University of Liège), D. Barrado (Centro de Astrobiología), Anthony Boccaletti (Centre National de la Recherche Scientifique, Université Paris Sciences et Lettres), Valentin Christiaens (University of Liège, KU Leuven), Danny Gasman (KU Leuven), Sierra L. Grant (Carnegie Institution for Science, Earth and Planets Laboratory), Hyerin Jang (Radboud University Nijmegen), Till Kaeufer (Austrian Academy of Sciences, University of Groningen), Jayatee Kanwar (Austrian Academy of Sciences, University of Groningen), Giulia Perotti (University of Copenhagen, Max Planck Institute for Astronomy), Kamber R. Schwarz (Max Planck Institute for Astronomy), Milou Temmink (Leiden University, Leiden Observatory)
Abstract: Abstract Mechanisms such as collisions of rocky bodies or cometary activity give rise to dusty debris disks. Debris disks trace the leftover building blocks of planets, and thus also planetary composition. HD 172555, a stellar twin of β Pic, hosts a debris disk thought to have resulted from a giant collision. It is known for its extreme mid-infrared silica dust feature, indicating a warm population of silica-rich grains in the asteroid belt (∼5 au), cold CO observed by Atacama Large Millimeter/submillimeter Array (ALMA), and small bodies evaporating as they approach close to the star. Our JWST Mid-InfraRed Instrument/Medium Resolution Spectroscopy (MIRI MRS) observations now reveal emission from an inner gaseous disk (<0.5 au) that arises from the evaporation of close-in material. For the first time in a debris disk, we detect neutral atomic chlorine and sulfur, as well as ionized nickel. We recovered the neutral sulfur line in ∼20 yr old Spitzer data, showing it is long-lived and stable. Ionized iron, previously seen only in β Pic, is also detected. All lines are broadened by Keplerian rotation, pinpointing the gas location. The HD 172555 system serves as a unique laboratory to study the composition of planetesimals, asteroids, and comets beyond the solar system. The comparison to β Pic reveals that the gas in HD 172555 is hotter, closer to the star, and poor in argon—suggesting it originates from evaporating rocky bodies near the star, while β Pic’s gas may trace volatile-rich bodies from larger separations.