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A New Mechanism for Forming Hot Corinos: Shocks from Binary Interactions Munan Gong Max Planck Institute for Extraterrestrial Physics (MPE) With Maria Jose Maureira, Paola Caselli, Joaquin Zamponi (MPE), Lorenz Gaertner (LMU), Kaitlin Kratter (Arizona), Kedron Silsbee (UTEP) Towards New Frontiers, ESO, 11 March, 2025
The deeply embedded Protostellar Disk IRAS 16293-2422 Slide credit: Maria Jose Maureira (MPE)
4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 Slide credit: Maria Jose Maureira (MPE) The deeply embedded Protostellar Disk IRAS 16293-2422
4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 Cazaux et al. (2003) …we conclude that the high abundance of complex species in the hot core around IRAS 16293 implies the evaporation of ice into the warm gas. — Cazaux et al. (2003) The First Detection of Complex Organic Molecule (COM) Emissions towards a Low Mass Protostar Caselli & Ceccarelli (2012) I review what we know today about the inner warm regions of solar type protostars. I will call these regions “hot corinos" to distinguish them from massive hot cores. — Ceccarelli et al. (2004)
I review what we know today about the inner warm regions of solar type protostars. I will call these regions “hot corinos" to distinguish them from massive hot cores. — Ceccarelli et al. (2004) High Mass Protostar + COM Emission = “Hot Core” Low Mass Protostar + COM Emission = “Hot Corino” 4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 Cazaux et al. (2003) …we conclude that the high abundance of complex species in the hot core around IRAS 16293 implies the evaporation of ice into the warm gas. — Cazaux et al. (2003) The Name of “Hot Corino” Caselli & Ceccarelli (2012)
4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 Physical Model of IRAS 16293 Doty et al. (2004), See also Schöier et al. (2002), Ceccarelli et a. (2000)
4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 Multiple Hot Corinos ALMA continuum Jorgensen et al. 2016, Maureira, Gong et al. 2020a 141 au Forest of COM lines Manigand et al. 2020 Spatial distribution of COMs poorly resolved Oya et al. 2018
4-6 Msun within few 1,000 au 0.14 pc Herschel column density! Ladjelate et al. 2020 ALMA continuum Jorgensen et al. 2016, Maureira, Gong et al. 2020a 141 au A Triple System: Binary + Companion ALMA continuum Jorgensen et al. 2016, Maureira et al. 2020, 2022 141 au
Hot Spots in the Circumbinary Disk of IRAS 16293 A Maureira et al. (2018) Maureira, Gong et al. (2022) •What is the origin of the hot spots?
Hints of Binary Shocks in Class 0/I Protostellar Disks Alves et al. (2019), Vastel et al. (2025) BHB2007, CH3OH emission near one spiral feature Hsieh et al. (2025) SVS13A, CH3CN emission in the “bridge” between two protostars
Take Home Messages: The Keys to Modelling Protostellar Disks I. Dynamics Rules Radiative Heating, Dust, Chemistry… + Young Disks are Not Passive Dynamical Effects: - Shocks (Maureira et al. 2022, Gong et al. in prep) - Accretion Heating (Zamponi et al. 2021, Lin et al. 2020) Disks are NOT isothermal/locally isothermal II. Simulation Needs Thermodynamics T ≠ constant It is Important to include heating and cooling in hydrodynamical simulations We need both high-resolution observations and realistic simulations III. Observation + Simulation
Q1: What causes hot spots in binary protostellar disks? •A. Aliens trying to get WIFI from their phones •B. Shocks created by the gravitational interaction between the gas and the binary stars Q2: How can we understand protostellar disks? •A. By conducting high resolution observations of dust and molecular lines •B. By building realistic numerical simulations with thermodynamics •C. By combining observations and simulations •D. All of the above Summary Quiz!
