The Impact of Cosmic Rays on the Kinematics of the Circumgalactic Medium

Butsky, Iryna S.; Werk, Jessica K.; Tchernyshyov, Kirill; Fielding, Drummond B.; Joseph, Breneman,; Piacitelli, Daniel; Quinn, Thomas; Sanchez, N. Nicole; Cruz, Akaxia; Hummels, Cameron B.; Burchett, Joseph N.; Tremmel, Michael

doi:10.3847/1538-4357/ac7ebd

Cited by 10 publications

(4 citation statements)

References 105 publications

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“…If the halo becomes CR dominated, the pressure support provided by CRs can potentially allow the cool, photoionized (T ∼ 10 4 K) phase to become volume-filling, with abundant Ovi ( Ji et al 2020), and suppression of virial shocks ( Ji et al 2021). Even if the gas remains multiphase, CR pressure support in cold clouds reduces their density and increases buoyancy, increasing free-fall times (Butsky et al 2020) and altering kinematic absorption-line signatures (Butsky et al 2022). Heating by CRs can also offset radiative cooling, though this has mostly been modeled in the ICM (Guo & Oh 2008, Jacob & Pfrommer 2017, Ruszkowski et al 2017.…”

Section: Cold Gas Interactions: Cosmic Raysmentioning

confidence: 99%

Key Physical Processes in the Circumgalactic Medium

Faucher-Giguère,

2023

Annual Review of Astronomy and Astrophysics

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Spurred by rich, multiwavelength observations and enabled by new simulations, ranging from cosmological to subparsec scales, the past decade has seen major theoretical progress in our understanding of the circumgalactic medium (CGM). We review key physical processes in the CGM. Our conclusions include the following: ▪ The properties of the CGM depend on a competition between gravity-driven infall and gas cooling. When cooling is slow relative to free fall, the gas is hot (roughly virial temperature), whereas the gas is cold ( T ∼ 104 K) when cooling is rapid. ▪ Gas inflows and outflows play crucial roles, as does the cosmological environment. Large-scale structure collimates cold streams and provides angular momentum. Satellite galaxies contribute to the CGM through winds and gas stripping. ▪ In multiphase gas, the hot and cold phases continuously exchange mass, energy, and momentum. The interaction between turbulent mixing and radiative cooling is critical. A broad spectrum of cold gas structures, going down to subparsec scales, arises from fragmentation, coagulation, and condensation onto gas clouds. ▪ Magnetic fields, thermal conduction, and cosmic rays can substantially modify how the cold and hot phases interact, although microphysical uncertainties are presently large. Key open questions for future work include the mutual interplay between small-scale structure and large-scale dynamics, and how the CGM affects the evolution of galaxies.

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Section: Cold Gas Interactions: Cosmic Raysmentioning

confidence: 99%

Key Physical Processes in the Circumgalactic Medium

Faucher-Giguère,

2023

Annual Review of Astronomy and Astrophysics

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“…Nelson et al (2018a) report a more direct connection between star formation and the transport of oxygen-enriched gas into the CGM by AGN feedback in IllustrisTNG. Such differences may be the tip of an iceberg, as the inclusion of physical processes not treated by either EAGLE or IllustrisTNG, for example, feedback by cosmic rays, may induce significant changes to the CGM , Butsky et al 2022.…”

Section: Physical Properties Of the Circumgalactic Mediummentioning

confidence: 99%

Hydrodynamical Simulations of the Galaxy Population: Enduring Successes and Outstanding Challenges

Crain

Voort

2023

Annual Review of Astronomy and Astrophysics

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We review the progress in modeling the galaxy population in hydrodynamical simulations of the ΛCDM cosmogony. State-of-the-art simulations now broadly reproduce the observed spatial clustering of galaxies; the distributions of key characteristics, such as mass, size, and SFR; and scaling relations connecting diverse properties to mass. Such improvements engender confidence in the insight drawn from simulations. Many important outcomes, however, particularly the properties of circumgalactic gas, are sensitive to the details of the subgrid models used to approximate the macroscopic effects of unresolved physics, such as feedback processes. We compare the outcomes of leading simulation suites with observations, and with each other, to identify the enduring successes they have cultivated and the outstanding challenges to be tackled with the next generation of models. Our key conclusions include the following: ▪ Realistic galaxies can be reproduced by calibrating the ill-constrained parameters of subgrid feedback models. Feedback is dominated by stars and black holes in low-mass and high mass galaxies, respectively. ▪ Adjusting or disabling the processes implemented in simulations can elucidate their impact on observables, but outcomes can be degenerate. ▪ Similar galaxy populations can emerge in simulations with dissimilar feedback implementations. However, these models generally predict markedly different gas flow rates into, and out of, galaxies and their halos. CGM observations are thus a promising means of breaking this degeneracy and guiding the development of new feedback models. Expected final online publication date for the Annual Review of Astronomy and Astrophysics, Volume 61 is August 2023. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

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“…The level of CR pressure support in the CGM may also be probed by observing systematic kinematic offsets between low and high ions (Butsky et al. 2022 ). While in CR-dominated halos the offset is relatively small, it can be substantial when CR pressure is negligible.…”

Section: Observational Signaturesmentioning

confidence: 99%

Cosmic ray feedback in galaxies and galaxy clusters

Ruszkowski,

Pfrommer

2023

Astron Astrophys Rev

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Understanding the physical mechanisms that control galaxy formation is a fundamental challenge in contemporary astrophysics. Recent advances in the field of astrophysical feedback strongly suggest that cosmic rays (CRs) may be crucially important for our understanding of cosmological galaxy formation and evolution. The appealing features of CRs are their relatively long cooling times and relatively strong dynamical coupling to the gas. In galaxies, CRs can be close to equipartition with the thermal, magnetic, and turbulent energy density in the interstellar medium, and can be dynamically very important in driving large-scale galactic winds. Similarly, CRs may provide a significant contribution to the pressure in the circumgalactic medium. In galaxy clusters, CRs may play a key role in addressing the classic cooling flow problem by facilitating efficient heating of the intracluster medium and preventing excessive star formation. Overall, the underlying physics of CR interactions with plasmas exhibit broad parallels across the entire range of scales characteristic of the interstellar, circumgalactic, and intracluster media. Here we present a review of the state-of-the-art of this field and provide a pedagogical introduction to cosmic ray plasma physics, including the physics of wave–particle interactions, acceleration processes, CR spatial and spectral transport, and important cooling processes. The field is ripe for discovery and will remain the subject of intense theoretical, computational, and observational research over the next decade with profound implications for the interpretation of the observations of stellar and supermassive black hole feedback spanning the entire width of the electromagnetic spectrum and multi-messenger data.

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The Impact of Cosmic Rays on the Kinematics of the Circumgalactic Medium

Cited by 10 publications

References 105 publications

Key Physical Processes in the Circumgalactic Medium

Key Physical Processes in the Circumgalactic Medium

Hydrodynamical Simulations of the Galaxy Population: Enduring Successes and Outstanding Challenges

Cosmic ray feedback in galaxies and galaxy clusters

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