TY - JOUR
T1 - The Launching of Cold Clouds by Galaxy Outflows. V. The Role of Anisotropic Thermal Conduction
AU - Brüggen, Marcus
AU - Scannapieco, Evan
AU - Grete, Philipp
N1 - Funding Information:
We thank Max Gronke, Ryan Farber, and Fernando Hidalgo-Pineda for valuable discussions, as well as the anonymous referee for a very constructive report. M.B. acknowledges support from the Deutsche Forschungsgemeinschaft under Germany’s Excellence Strategy—EXC 2121 “Quantum Universe”—390833306 and the support and collaboration with the Center for Data and Computing in Natural Sciences (CDCS). E.S. acknowledges support from the NASA grant 80NSSC22K1265. This project has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101030214. We would like to thank the Kavli Institute for Theoretical Physics and the organizers of the workshops Fundamentals of Gaseous Halos (Halo21) and The Cosmic Web: Connecting Galaxies to Cosmology at High and Low Redshift (CosmicWeb23). This research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958. Part of the simulations were run on the JUWELS supercomputer at the Jülich Center for Supercomputing within the project ANISOCOND.
Funding Information:
We thank Max Gronke, Ryan Farber, and Fernando Hidalgo-Pineda for valuable discussions, as well as the anonymous referee for a very constructive report. M.B. acknowledges support from the Deutsche Forschungsgemeinschaft under Germany’s Excellence Strategy—EXC 2121 “Quantum Universe”—390833306 and the support and collaboration with the Center for Data and Computing in Natural Sciences (CDCS). E.S. acknowledges support from the NASA grant 80NSSC22K1265. This project has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101030214. We would like to thank the Kavli Institute for Theoretical Physics and the organizers of the workshops Fundamentals of Gaseous Halos (Halo21) and The Cosmic Web: Connecting Galaxies to Cosmology at High and Low Redshift (CosmicWeb23). This research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958. Part of the simulations were run on the JUWELS supercomputer at the Jülich Center for Supercomputing within the project ANISOCOND.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/7/1
Y1 - 2023/7/1
N2 - Motivated by observations of multiphase galaxy outflows, we explore the impact of isotropic and anisotropic electron thermal conduction on the evolution of radiatively cooled, cold clouds embedded in hot, magnetized winds. Using the adaptive-mesh refinement code AthenaPK, we conduct simulations of clouds impacted by supersonic and transonic flows with magnetic fields initially aligned parallel and perpendicular to the flow direction. In cases with isotropic thermal conduction, an evaporative wind forms, stabilizing against instabilities and leading to a mass-loss rate that matches the hydrodynamic case. In anisotropic cases, the impact of conduction is more limited and strongly dependent on the field orientation. In runs with initially perpendicular fields, the field lines are folded back into the tail, strongly limiting conduction, but magnetic fields act to dampen instabilities and slow the stretching of the cloud in the flow direction. In the parallel case, anisotropic conduction aids cloud survival by forming a radiative wind near the front of the cloud, which suppresses instabilities and reduces mass loss. In all cases, anisotropic conduction has a minimal impact on the acceleration of the cloud.
AB - Motivated by observations of multiphase galaxy outflows, we explore the impact of isotropic and anisotropic electron thermal conduction on the evolution of radiatively cooled, cold clouds embedded in hot, magnetized winds. Using the adaptive-mesh refinement code AthenaPK, we conduct simulations of clouds impacted by supersonic and transonic flows with magnetic fields initially aligned parallel and perpendicular to the flow direction. In cases with isotropic thermal conduction, an evaporative wind forms, stabilizing against instabilities and leading to a mass-loss rate that matches the hydrodynamic case. In anisotropic cases, the impact of conduction is more limited and strongly dependent on the field orientation. In runs with initially perpendicular fields, the field lines are folded back into the tail, strongly limiting conduction, but magnetic fields act to dampen instabilities and slow the stretching of the cloud in the flow direction. In the parallel case, anisotropic conduction aids cloud survival by forming a radiative wind near the front of the cloud, which suppresses instabilities and reduces mass loss. In all cases, anisotropic conduction has a minimal impact on the acceleration of the cloud.
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U2 - 10.3847/1538-4357/acd63e
DO - 10.3847/1538-4357/acd63e
M3 - Article
AN - SCOPUS:85164961067
SN - 0004-637X
VL - 951
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 113
ER -