Outflows from starburst galaxies with various driving mechanisms and their X-ray properties

Yu, B. P. Brian; Owen, Ellis R.; Pan, K.; Wu, Kinwah; Ferreras, Ignacio

doi:10.1093/mnras/stab2738

Cited by 5 publications

(4 citation statements)

References 116 publications

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“…CRs can play a key role in driving galactic outflows [15,512,[646][647][648][649][650][651][652]. Their influence leads to modifications in the flow dynamics and physical properties [15,480,598,653,654] which can be observed in various ways, including with X-rays [655] or with Lyman-α spectra [656]. Recent numerical studies have extensively explored CR-driven winds.…”

Section: Cosmic Ray Impacts On Galactic Outflow Physicsmentioning

confidence: 99%

Cosmic Ray Processes in Galactic Ecosystems

Owen

Inoue

et al. 2023

Galaxies

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Galaxy evolution is an important topic, and our physical understanding must be complete to establish a correct picture. This includes a thorough treatment of feedback. The effects of thermal–mechanical and radiative feedback have been widely considered; however, cosmic rays (CRs) are also powerful energy carriers in galactic ecosystems. Resolving the capability of CRs to operate as a feedback agent is therefore essential to advance our understanding of the processes regulating galaxies. The effects of CRs are yet to be fully understood, and their complex multi-channel feedback mechanisms operating across the hierarchy of galaxy structures pose a significant technical challenge. This review examines the role of CRs in galaxies, from the scale of molecular clouds to the circumgalactic medium. An overview of their interaction processes, their implications for galaxy evolution, and their observable signatures is provided and their capability to modify the thermal and hydrodynamic configuration of galactic ecosystems is discussed. We present recent advancements in our understanding of CR processes and interpretation of their signatures, and highlight where technical challenges and unresolved questions persist. We discuss how these may be addressed with upcoming opportunities.

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Section: Cosmic Ray Impacts On Galactic Outflow Physicsmentioning

confidence: 99%

Cosmic Ray Processes in Galactic Ecosystems

Owen

Inoue

et al. 2023

Galaxies

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“…The remainder is therefore available to drive an outflow. Following the fiducial choices of [16], we take the CR and thermal powers to be equal, i.e. 𝐸 = 𝛼 𝐸 tot , 𝐸 c = 𝛼 c 𝐸 tot , and 𝐿 0 = 𝛼 L 𝐸 tot , where 𝛼 = 0.05, 𝛼 c = 0.05, and 𝛼 L = 0.9.…”

Section: Pos(icrc2023)554mentioning

confidence: 99%

Cosmic ray calorimetry in star-forming galaxy populations and implications for their contribution to the extra-galactic 𝜸-ray background

Owen¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

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Star-forming galaxies (SFGs) have been established as an important source population in the extra-galactic 𝛾-ray background (EGB). Their intensive star-formation creates an abundance of environments able to accelerate particles, and these build-up a rich sea of cosmic rays (CRs). Above GeV energies, CR protons can undergo hadronic interactions with their environment to produce 𝛾-rays. SFGs can operate as CR proton "calorimeters", where a large fraction of the CR energy is converted to 𝛾-rays. However, CRs also deposit energy and momentum to modify the thermal and hydrodynamic conditions of the gas in SFGs, and can become a powerful driver of outflows. Such outflows are ubiquitous among some types of SFGs, and have the potential to severely degrade their CR proton calorimetry. This diminishes their contribution to the EGB. In this work, we adopt a self-consistent treatment of particle transport in outflows from SFGs to assess their calorimetry. We use 1D numerical treatments of galactic outflows driven by CRs and thermal gas pressure, accounting for the dynamical effects and interactions of CRs. We show the impact CR-driven flows have on the relative contribution of SFG populations to the EGB, and investigate the properties of SFGs that contribute most strongly.

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“…The evolution of these wind bubbles is somewhat analogous to stellar bubbles, but on galactic scales. The wind bubble dynamics have been studied analytically (Castor et al 1975;Weaver et al 1977;Koo & McKee 1992) and through simulations (Tenorio-Tagle & Muñoz-Tuñón 1997;Strickland & Stevens 2000;Strickland et al 2002;Melioli et al 2013;Fielding et al 2017;Schneider et al 2020;Yu et al 2021;Nguyen & Thompson 2022), but several aspects of the dynamical evolution still remain unclear (Lancaster et al 2021a,b), especially the influence of the galactic disk and the large-scale magnetic field.…”

Section: Introductionmentioning

confidence: 99%

The galactic bubbles of starburst galaxies

Meliani,

Cristofari,

Rodríguez-González

et al. 2024

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The galactic winds of starburst galaxies (SBGs) give rise to remarkable structures on kiloparsec scales. However, the evolution and shape of these giant wind bubbles, as well as the properties of the shocks they develop, are not yet fully understood. We aim to understand what shapes the galactic winds of SBGs, with a particular focus on the role of large-scale magnetic fields in the dynamical evolution of galactic wind-inflated bubbles. In addition, we aim to explore where the conditions for efficient particle acceleration are met in these systems. We performed magnetohydrodynamic simulations with the AMRVAC code (Adaptive Mesh Refinement Versatile Advection Code) with various configurations of the galactic medium density profile and magnetization. We observe that the large-scale magnetic field, in which galactic winds expand, can impact the structure and evolution of inflated bubbles. However, the typical structures observed in starburst galaxies, such as M82, cannot be solely explained by the magnetic field structures that have been considered. This highlights the importance of other factors, such as the galactic disk, in shaping the galactic bubble. Furthermore, in all the magnetized cases we investigated, the forward wave resulting from the expanding bubbles only results in compression waves, whereas the wind termination shock features high Mach numbers, making it a promising site for diffusive shock acceleration up to $ PeV$. The synthetic X-ray images generated from our models reveal an envelope surrounding the bubbles that extends up to 2 kpc, which could correspond to the polarized emission observed from planar geometry in M82, as well as a large structure inside the bubble corresponding to the shocked galactic wind. Additionally, our findings indicate that, as observed with the SOFIA instrument, a large ordered magnetic field is associated with the free galactic wind, while a more turbulent magnetic field is present in the shocked region.

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Outflows from starburst galaxies with various driving mechanisms and their X-ray properties

Cited by 5 publications

References 116 publications

Cosmic Ray Processes in Galactic Ecosystems

Cosmic Ray Processes in Galactic Ecosystems

Cosmic ray calorimetry in star-forming galaxy populations and implications for their contribution to the extra-galactic 𝜸-ray background

The galactic bubbles of starburst galaxies

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