Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations

Woorak Choi, Chang Goo Kim, Aeree Chung

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Ram pressure stripping (RPS) is a process that removes the interstellar medium (ISM) quickly, playing a vital role in galaxy evolution. Previous RPS studies have treated the ISM as single-phase or lack the resolution and physical processes to properly capture the full multiphase ISM. To improve this simplification, we introduce an inflowing, hot intracluster medium (ICM) into a self-consistently modeled ISM in a local patch of star-forming galactic disks using the TIGRESS framework. Our simulations reveal that the workings of RPS are not only direct acceleration of the ISM by ICM ram pressure but also mixing-driven momentum transfer involving significant phase transition and radiative cooling. The hot ICM passes through the low-density channels of the porous, multiphase ISM; shreds the cool ISM; and creates mixing layers. The ICM momentum is transferred through the mixing layers while populating the intermediate-temperature gas and radiating thermal energy away. The mixed gas extends beyond galactic disks and forms stripped tails that cool back unless the ICM fluxes are large enough to prevent cooling until they escape the simulation domain. The mixing-driven momentum transfer predicts that the more ICM mixes in, the faster the ISM moves, resulting in the anticorrelation of outflow velocity and gas metallicity of the stripped ISM. The compression of the ISM disks due to the ICM ram pressure enhances star formation rates up to 50% compared to the model without ICM. With the ICM ram pressure higher than the disk anchoring pressure, star formation is quenched within 1/4100 Myr.

Original languageEnglish
Article number133
JournalAstrophysical Journal
Issue number2
Publication statusPublished - 2022 Sept 1

Bibliographical note

Funding Information:
We acknowledge the anonymous referee for comments and suggestions that improved the clarity and quality of this paper. A.C. and W.C. acknowledge support by the National Research Foundation of Korea (NRF), grant Nos. 2018R1D1A1B07048314, 2022R1A2C100298211, and 2022R1A6A1A03053472. C.-G.K. was supported by the National Aeronautics and Space Administration (NASA) through ATP grant No. NNX17AG26G and Chandra Award No. TM0-21009X. Resources supporting this work were provided in part by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center and in part by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Office of Information Technology’s High Performance Computing Center.

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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