Star Formation Triggered by Feedback from Massive Stars

Walch, Stefanie

doi:10.1007/978-3-319-03041-8_32

Cited by 5 publications

(3 citation statements)

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“…Silk 2013; Bieri et al 2015, though the engine here is massive stars rather than AGNs) and the 'triggered star formation' model 8 (e.g. Elmegreen & Lada 1977;Palous et al 1994;Elmegreen et al 2002;Whitworth & Francis 2002;Tan 2000Tan , 2005Walch 2014). Finally, feedback from the starburst eventually blows out almost all the gas from the central region and thus star formation is temporarily suppressed in the galaxy (panel F).…”

Section: Gc Formation In High-pressure Cloudsmentioning

confidence: 99%

Self-consistent proto-globular cluster formation in cosmological simulations of high-redshift galaxies

Grudić

Quataert

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report the formation of bound star clusters in a sample of high-resolution cosmological zoom-in simulations of z 5 galaxies from the FIRE project. We find that bound clusters preferentially form in high-pressure clouds with gas surface densities over 10 4 M pc −2 , where the cloud-scale star formation efficiency is near unity and young stars born in these regions are gravitationally bound at birth. These high-pressure clouds are compressed by feedback-driven winds and/or collisions of smaller clouds/gas streams in highly gas-rich, turbulent environments. The newly formed clusters follow a power-law mass function of dN/dM ∼ M −2 . The cluster formation efficiency is similar across galaxies with stellar masses of ∼ 10 7 -10 10 M at z 5. The age spread of cluster stars is typically a few Myrs and increases with cluster mass. The metallicity dispersion of cluster members is ∼ 0.08 dex in [Z/H] and does not depend on cluster mass significantly. Our findings support the scenario that present-day old globular clusters (GCs) were formed during relatively normal star formation in high-redshift galaxies. Simulations with a stricter/looser star formation model form a factor of a few more/fewer bound clusters per stellar mass formed, while the shape of the mass function is unchanged. Simulations with a lower local star formation efficiency form more stars in bound clusters. The simulated clusters are larger than observed GCs due to finite resolution. Our simulations are among the first cosmological simulations that form bound clusters self-consistently in a wide range of high-redshift galaxies.

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Section: Gc Formation In High-pressure Cloudsmentioning

confidence: 99%

Self-consistent proto-globular cluster formation in cosmological simulations of high-redshift galaxies

Grudić

Quataert

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…In some cases it can also sweep up or induce material to form a subsequent generation of stars (see, for instance Liu et al 2014;Bisbas et al 2011). Furthermore, it is the principal process by which molecular clouds are destroyed (Matzner 2002), and how quickly this occurs dictates the impact and propagation of material from supernovae into the cloud and surrounding intertstellar medium (ISM; Walch 2014;Iffrig & Hennebelle 2015). The progress of this ionising feedback therefore has a profound effect on the star formation cycle from cloud core to Galactic scales (e.g.…”

Section: Introductionmentioning

confidence: 99%

Carina’s pillars of destruction: the view from ALMA

Klaassen

Reiter

McLeod

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Forming high-mass stars have a significant effect on their natal environment. Their feedback pathways, including winds, outflows, and ionising radiation, shape the evolution of their surroundings which impacts the formation of the next generation of stars. They create or reveal dense pillars of gas and dust towards the edges of the cavities they clear. They are modelled in feedback simulations, and the sizes and shapes of the pillars produced are consistent with those observed. However, these models predict measurably different kinematics which provides testable discriminants. Here we present the first ALMA Compact Array (ACA) survey of 13 pillars in Carina, observed in 12 CO, 13 CO and C 18 O J=2-1, and the 230 GHz continuum. The pillars in this survey were chosen to cover a wide range in properties relating to the amount and direction of incident radiation, proximity to nearby irradiating clusters and cloud rims, and whether they are detached from the cloud. With these data, we are able to discriminate between models. We generally find pillar velocity dispersions of < 1 km s −1 and that the outer few layers of molecular emission in these pillars show no significant offsets from each other, suggesting little bulk internal motions within the pillars. There are instances where the pillars are offset in velocity from their parental cloud rim, and some with no offset, hinting at a stochastic development of these motions.

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“…Implosion is the process by which an object is destroyed by being forced to close in on itself. Implosions have many scientific applications such as how gas bubbles, sites for chemical reactions, are eliminated inside of fluids [1], the formation and collapse of stars [2], or even the demolition of buildings [3]. There has been mathematical interest in their study such as in finding exact similarity solutions to the porous media equations subject to fixed spatial pressure functions [4], and in studying the stability of similarity solutions in the presence of perturbations [5].…”

Section: Introductionmentioning

confidence: 99%

Assessment of the effects of azimuthal mode number perturbations upon the implosion processes of fluids in cylinders

Lindstrom

2017

Physica D: Nonlinear Phenomena

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Fluid instabilities arise in a variety of contexts and are often unwanted results of engineering imperfections. In one particular model for a magnetized target fusion reactor, a pressure wave is propagated in a cylindrical annulus comprised of a dense fluid before impinging upon a plasma and imploding it. Part of the success of the apparatus is a function of how axially-symmetric the final pressure pulse is upon impacting the plasma. We study a simple model for the implosion of the system to study how imperfections in the pressure imparted on the outer circumference grow due to geometric focusing. Our methodology entails linearizing the compressible Euler equations for mass and momentum conservation about a cylindrically symmetric problem and analyzing the perturbed profiles at different mode numbers. The linearized system gives rise to singular shocks and through analyzing the perturbation profiles at various times, we infer that high mode numbers are dampened through the propagation. We also study the Linear Klein-Gordon equation in the context of stability of linear cylindrical wave formation whereby highly oscillatory, bounded behaviour is observed in a far field solution.

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Star Formation Triggered by Feedback from Massive Stars

Cited by 5 publications

References 0 publications

Self-consistent proto-globular cluster formation in cosmological simulations of high-redshift galaxies

Self-consistent proto-globular cluster formation in cosmological simulations of high-redshift galaxies

Carina’s pillars of destruction: the view from ALMA

Assessment of the effects of azimuthal mode number perturbations upon the implosion processes of fluids in cylinders

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