Cosmic rays in galaxy halos I: the circumgalactic transport rate and a dynamically significant cosmic-ray reservoir
Abstract
Fermi-LAT observations imply that most of the cosmic rays (CRs) produced in normal star-forming galaxies escape from the discs where they are accelerated into the circumgalactic medium (CGM), but the subsequent evolution of those escaping CRs is unclear. Here we construct a simple semi-analytic model for their transport and loss, which we constrain by confronting the model with a series of observations: limits on CR energy densities in the outer Milky Way from Fermi-LAT, the isotropic gamma-ray background (IGRB), stacked CGM X-ray emission from eROSITA, and the requirement that the accumulated pressure of CRs in galaxy CGMs not be so large as to render them unstable. We show that these constraints can be jointly satisfied in only two scenarios: one where CRs diffuse quickly through the CGM and freely escape beyond it into the IGM, and another where the CR diffusion time out of halos is of order the Hubble time. In the latter scenario CRs accelerated by star formation naturally explain both the IGRB and the heat input required to maintain the temperature of the CGM against X-ray cooling, and their relatively slow transport means that roughly half of the CR energy injected into the CGM of an L⋆ halo over its star-formation history remains there at z ≃ 0. This makes CR pressure dynamically significant, and also means that a non-negligible part of the IGRB is produced by CRs in the Milky Way's own halo. We argue that this latter scenario is the more likely one, as it avoids the need to posit a second source for the IGRB that is coincidentally very close in both power and spectral shape to the contribution from star-forming discs.
Related
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BibTeX
@misc{crocker2026cosmic,
title = {{Cosmic rays in galaxy halos I: the circumgalactic transport rate and a dynamically significant cosmic-ray reservoir}},
author = {Roland M. Crocker and Mark R. Krumholz},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.38061},
eprint = {2610.38061},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.38061},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Cosmic rays in galaxy halos I: the circumgalactic transport rate and a dynamically significant cosmic-ray reservoir
AU - Roland M. Crocker
AU - Mark R. Krumholz
PY - 2026
DA - 2026/10/27
PB - arXiv
DO - 10.48550/arxiv.2610.38061
UR - https://arxiv.org/abs/2610.38061
AB - Fermi-LAT observations imply that most of the cosmic rays (CRs) produced in normal star-forming galaxies escape from the discs where they are accelerated into the circumgalactic medium (CGM), but the subsequent evolution of those escaping CRs is unclear. Here we construct a simple semi-analytic model for their transport and loss, which we constrain by confronting the model with a series of observations: limits on CR energy densities in the outer Milky Way from Fermi-LAT, the isotropic gamma-ray background (IGRB), stacked CGM X-ray emission from eROSITA, and the requirement that the accumulated pressure of CRs in galaxy CGMs not be so large as to render them unstable. We show that these constraints can be jointly satisfied in only two scenarios: one where CRs diffuse quickly through the CGM and freely escape beyond it into the IGM, and another where the CR diffusion time out of halos is of order the Hubble time. In the latter scenario CRs accelerated by star formation naturally explain both the IGRB and the heat input required to maintain the temperature of the CGM against X-ray cooling, and their relatively slow transport means that roughly half of the CR energy injected into the CGM of an L_⋆ halo over its star-formation history remains there at z ≃ 0. This makes CR pressure dynamically significant, and also means that a non-negligible part of the IGRB is produced by CRs in the Milky Way's own halo. We argue that this latter scenario is the more likely one, as it avoids the need to posit a second source for the IGRB that is coincidentally very close in both power and spectral shape to the contribution from star-forming discs.
ER -