# Cosmic-Ray Driven Outflows to Mpc Scales from L* Galaxies

@article{Hopkins2020CosmicRayDO,
title={Cosmic-Ray Driven Outflows to Mpc Scales from L* Galaxies},
author={Philip F. Hopkins and T. K. Chan and Suoqing Ji and Cameron B. Hummels and Dus̆an Keres̆ and Eliot Quataert and Claude-Andr{\'e} Faucher-Gigu{\e}re},
journal={arXiv: Astrophysics of Galaxies},
year={2020}
}`
We study the effects of cosmic rays (CRs) on outflows from star-forming galaxies in the circum and inter-galactic medium (CGM/IGM), in high-resolution, fully-cosmological FIRE-2 simulations (accounting for mechanical and radiative stellar feedback, magnetic fields, anisotropic conduction/viscosity/CR diffusion and streaming, and CR losses). We showed previously that massive ($M_{\rm halo}\gtrsim 10^{11}\,M_{\odot}$), low-redshift ($z\lesssim 1-2$) halos can have CR pressure dominate over… Expand
10 Citations

#### Paper Mentions

Catch Me if You Can: Biased Distribution of Lyα-emitting Galaxies according to the Viewing Direction
We report that Lyα-emitting galaxies (LAEs) may not faithfully trace the cosmic web of neutral hydrogen (H i), but their distribution is likely biased depending on the viewing direction. We calculateExpand
Cosmic rays and non-thermal emission in simulated galaxies − I. Electron and proton spectra compared to Voyager-1 data
• Physics
• 2021
Current-day cosmic ray (CR) propagation studies use static Milky-Way models and fit parametrized source distributions to data. Instead, we use three-dimensional magneto-hydrodynamical (MHD)Expand
Cosmic-Ray Diffusion Suppression in Star-forming Regions Inhibits Clump Formation in Gas-rich Galaxies
• Physics
• The Astrophysical Journal
• 2021
Observations of the γ-ray emission around star clusters, isolated supernova remnants, and pulsar wind nebulae indicate that the cosmic-ray (CR) diffusion coefficient near acceleration sites can beExpand
MusE GAs FLOw and Wind V. The dust/metallicity-anisotropy of the circum-galactic medium
• Physics
• 2021
Based on 13 galaxy-MgII absorber pairs (9 - 81 kpc distance) from the MusE GAs FLOw and Wind (MEGAFLOW) survey at 0.4 0.8 along the minor axis. Given that [Zn/Fe] is a good proxy for metallicity,Expand
The Impact of Low-luminosity AGNs on Their Host Galaxies: A Radio and Optical Investigation of the Kiloparsec-scale Outflow in MaNGA 1-166919
• Physics
• 2021
One way an active galactic nucleus (AGN) influences the evolution of their host galaxy is by generating a large-scale (kiloparsec-scale) outflow. The content, energetics, and impact of such outflowsExpand
The relationship between gas and galaxies at z < 1 using the Q0107 quasar triplet
We study the distribution and dynamics of the circumand intergalactic medium using a dense galaxy survey covering the field around the Q0107 system, a unique z ≈ 1 projected quasar triplet. With fullExpand
Virialization of the Inner CGM in the FIRE Simulations and Implications for Galaxy Disks, Star Formation, and Feedback
We use the FIRE-2 cosmological simulations to study the formation of a quasi-static, virial-temperature gas phase in the circumgalactic medium (CGM) at redshifts 0 < z < 5 and how the formation ofExpand
Constraining magnetic fields in the circumgalactic medium
• Physics
• Monthly Notices of the Royal Astronomical Society
• 2020
We study the properties of magnetic fields in the circumgalactic medium (CGM) of z < 1 galaxies by correlating Faraday rotation measures (RMs) of ∼1000 high-redshift radio sources with theExpand
Gamma-Ray and Radio Background Constraints on Cosmic Rays in Milky Way Circumgalactic Medium
• Physics
• 2020
We study the interaction of cosmic rays (CRs) with the diffuse circumgalactic gas of Milky Way (MW) galaxy that results in hadronic $\gamma-$ray emission and radio synchrotron emission. We aim toExpand
Unravelling the physics of multiphase AGN winds through emission line tracers
• Physics
• 2020
Observations of emission lines in Active Galactic Nuclei (AGN) often find fast (~1000 km s^-1) outflows extending to kiloparsec scales, seen in ionised, neutral atomic and molecular gas. In this workExpand

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