Starburst and post-starburst high-redshift protogalaxies

Owen, Ellis R.; Wu, Kinwah; Jin, X.; Surajbali, P.; Kataoka, Noriko

doi:10.1051/0004-6361/201834350

Cited by 26 publications

(38 citation statements)

References 253 publications

(324 reference statements)

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“…Devine & Bally 1999;Tsuru et al 2007) is substantially shorter than the duration of the starburst episode driving it (∼100s of Myr, e.g. McQuinn et al 2010;Hashimoto et al 2018;McQuinn et al 2018;Owen et al 2019b), a result supported by observations. This means that the mass and energy injection rates remain roughly steady, and a stationary outflow can therefore develop.…”

Section: Additional Remarksmentioning

confidence: 77%

A hydrodynamical study of outflows in starburst galaxies with different driving mechanisms

Owen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Outflows from starburst galaxies can be driven by thermal pressure, radiation and cosmic rays. We present an analytic phenomenological model that accounts for these contributions simultaneously to investigate their effects on the hydrodynamical properties of outflows. We assess the impact of energy injection, wind opacity, magnetic field strength and the mass of the host galaxy on flow velocity, temperature, density and pressure profiles. For an M82-like wind, a thermally-dominated driving mechanism is found to deliver the fastest and hottest wind. Radiation-driven winds in typical starburst-galaxy configurations are unable to attain the higher flow velocities and temperatures associated with thermal and cosmic ray-driven systems, leading to higher wind densities which would be more susceptible to cooling and fragmentation at lower altitudes. High opacity winds are more sensitive to radiative driving, but terminal flow velocities are still lower than those achieved by other driving mechanisms at realistic opacities. We demonstrate that variations in the outflow magnetic field can influence its coupling with cosmic rays, where stronger fields enable greater streaming but less driving near the base of the flow, instead with cosmic rays redirecting their driving impact to higher altitudes. The gravitational potential is less important in M82-like wind configurations, and substantial variations in the flow profiles only emerge at high altitude in massive haloes. This model offers a more generalised approach to examine the large scale hydrodynamical properties for a wide variety of starburst galaxies.

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Section: Additional Remarksmentioning

confidence: 77%

A hydrodynamical study of outflows in starburst galaxies with different driving mechanisms

Owen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…CR heating has been argued to be important in the ISM of galaxies (Field et al 1969;Wiener et al 2013b;Walker 2016;Owen et al 2018Owen et al , 2019b in their circumgalactic environments (e.g., Salem et al 2016;Owen et al 2019aOwen et al , 2019b, and even in the intra-cluster medium between galaxies (e.g., Loewenstein et al 1991;Wiener et al 2013a;Ruszkowski et al 2017). Its power is mediated by the thermalization mechanism(s) at work, as governed by the local conditions (e.g., density, ionization fraction, magnetic field).…”

Section: Heatingmentioning

confidence: 99%

“…Other mechanisms have also been proposed, but are unlikely to be as important as MHD wave damping, in particular, see Colafrancesco & Marchegiani (2008), Ruszkowski et al (2017), and Owen et al (2018, 2019b, where on 0.1 kpc scales, thermalization by Coulomb interactions in an ionized ISM is considered. In this process, secondary CRs are injected by pp interactions of CR primary protons (primary electrons would cool too quickly to propagate far from their source) to provide a channel by which CR protons can thermalize.…”

Section: Heatingmentioning

confidence: 99%

Observational Signatures of Cosmic-Ray Interactions in Molecular Clouds

Owen

Lai

et al. 2021

ApJ

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We investigate ionization and heating of gas in the dense, shielded clumps/cores of molecular clouds bathed by an influx of energetic, charged cosmic rays (CRs). These molecular clouds have complex structures, with substantial variation in their physical properties over a wide range of length scales. The propagation and distribution of CRs is thus regulated accordingly, in particular, by the magnetic fields threaded through the clouds and into the dense regions within. We have found that a specific heating rate reaching 10 −26 erg cm −3 s −1 can be sustained in the dense clumps/cores for Galactic environments, and this rate increases with CR energy density. The propagation of CRs and heating rates in some star-forming filaments identified in IC 5146 are calculated, with the CR diffusion coefficients in these structures determined from magnetic field fluctuations inferred from optical and near-infrared polarizations of starlight, which is presumably a magnetic field tracer. Our calculations indicate that CR heating can vary by nearly three orders of magnitude between different filaments within a cloud due to different levels of CR penetration. The CR ionization rate among these filaments is similar. The equilibrium temperature that could be maintained by CR heating alone is of order 1 K in a Galactic environment, but this value would be higher in strongly star-forming environments, thus causing an increase in the Jeans mass of their molecular clouds.

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“…This is governed by the spatial distribution of photons, including both those from the CMB and stellar radiation fields. For compact regions near the galaxy core, starbursts exhibit an energy density in their stellar radiation fields which may exceed (or be comparable to) that of the CMB, but at the superwind scale starlight is expected to have a negligible energy density compared to that of the CMB [72,73].…”

Section: Model Uptakementioning

confidence: 99%