Hadronic Interactions of Energetic Charged Particles in Protogalactic Outflow Environments and Implications for the Early Evolution of Galaxies

2019/01/04 by Ellis R. Owen, Xiangyu Jin, Kinwah Wu +1 · 1 citation
Physics and Astronomy · #Accretion (finance) #Advection #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cosmic ray #Dark Matter and Cosmic Phenomena #Diffusion #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Interstellar medium #Outflow #Physics #Redshift #Star formation #Supernova #astro-ph.GA #astro-ph.HE

paper · pdf · doi:10.1093/mnras/stz060

published as MNRAS 484, 1645-1671 (2019) · 29 pages, 16 figures, accepted for publication in MNRAS. v2: updated to match published version (reference added, minor typos corrected)

openalex publication_date 2019/01/04 · arxiv created 2019/02/05 · arxiv updated 2019/02/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

We investigate the interactions of energetic hadronic particles with the media in outflows from star-forming protogalaxies. These particles undergo pion-producing interactions which can drive a heating effect in the outflow, while those advected by the outflow also transport energy beyond the galaxy, heating the circumgalactic medium. We investigate how this process evolves over the length of the outflow and calculate the corresponding heating rates in advection-dominated and diffusion-dominated cosmic ray transport regimes. In a purely diffusive transport scenario, we find the peak heating rate reaches |10^-26 \rm erg~cm^-3 \rm s^-1| at the base of the outflow where the wind is driven by core-collapse supernovae at an event rate of 0.1 yr−1, but does not extend beyond 2 kpc. In the advection limit, the peak heating rate is reduced to |10^-28 \rm erg~cm^-3 \rm s^-1|⁠, but its extent can reach to tens of kpc. Around 10 per cent of the cosmic rays injected into the system can escape by advection with the outflow wind, while the remaining cosmic rays deliver an important interstellar heating effect. We apply our cosmic ray heating model to the recent observation of the high-redshift galaxy MACS1149-JD1 and show that it could account for the quenching of a previous starburst inferred from spectroscopic observations. Re-ignition of later star-formation may be caused by the presence of filamentary circumgalactic inflows which are reinstated after cosmic ray heating has subsided.

Citations

• Gamma-ray sky points to radial gradients in cosmic-ray transport
• Spectral Decline of PeV Neutrinos from Starburst Galaxies
• Strangulation as the primary mechanism for shutting down star formation in galaxies
• The Starburst Contribution to the Extragalactic γ‐Ray Background
• Suppression of star formation in the galaxy NGC 253 by a starburst-driven molecular wind
• Lyα-driven outflows around star-forming galaxies
• Indications of Proton-Dominated Cosmic-Ray Composition above 1.6 EeV
• VLBI Images of 49 Radio Supernovae in Arp 220
• The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types
• FermiLarge Area Telescope observations of Local Group galaxies: detection of M 31 and search for M 33
• Kinematic Masses of Super–Star Clusters in M82 from High‐Resolution Near‐Infrared Spectroscopy
• Parametrizations of inclusive cross sections for pion production in proton-proton collisions
• Models of high redshift luminosity functions and galactic outflows: The dependence on halo mass function
• Supernova feedback in an inhomogeneous interstellar medium
• The Formation of the First Star in the Universe
• Metal Enrichment of the Intergalactic Medium atz = 3 by Galactic Winds
• A Kinematic Link Between Boxy Bulges, Stellar Bars, and Nuclear Activity in NGC 3079 and NGC 4388
• On the Maximum Luminosity of Galaxies and Their Central Black Holes: Feedback from Momentum‐driven Winds
• The Formation of the First Stars. I. The Primordial Star‐forming Cloud
• How Massive Single Stars End Their Life
• Highly efficient star formation in NGC 5253 possibly from stream-fed accretion
• Radioactive 26Al from massive stars in the Galaxy
• The Astrophysics of Ultrahigh-Energy Cosmic Rays
• THE RADIAL AND AZIMUTHAL PROFILES OF Mg II ABSORPTION AROUND 0.5 <z< 0.9 zCOSMOS GALAXIES OF DIFFERENT COLORS, MASSES, AND ENVIRONMENTS
• Cosmic-Ray Propagation and Interactions in the Galaxy
• Radio Emission from Normal Galaxies
• Cosmic ray driven outflows from high-redshift galaxies
• ON THE GeV AND TeV DETECTIONS OF THE STARBURST GALAXIES M82 AND NGC 253
• Magnetic field seeding by galactic winds
• The death of massive stars - I. Observational constraints on the progenitors of Type II-P supernovae
• Progenitors of Core-Collapse Supernovae
• RESISTIVE MAGNETIC FIELD GENERATION AT COSMIC DAWN
• Molecular Gas and the Young Starburst in NGC 5253 Revisited
• Constraints on cosmic-ray efficiency in the supernova remnant RCW 86 using multi-wavelength observations
• Large-scale magnetized outflows from the Virgo Cluster spiral NGC 4569
• Efficient cold outflows driven by cosmic rays in high-redshift galaxies and their global effects on the IGM
• Resolved magnetic dynamo action in the simulated intracluster medium
• Galactic Winds
• Review of Multibody Charm Analyses
• HST/WFC3 OBSERVATIONS OF AN OFF-NUCLEAR SUPERBUBBLE IN ARP 220
• Galactic Winds and the Role Played by Massive Stars
• Time-dependent galactic winds

Cited by

• Cosmic ray neutrons in magnetized astrophysical structures