Winds in Star Clusters Drive Kolmogorov Turbulence

Gallegos-Garcia, Monica; Burkhart, Blakesley; Rosen, Anna L.; Naiman, Jill; Ramírez-Ruiz, E.

doi:10.3847/2041-8213/ababae

Cited by 23 publications

(20 citation statements)

References 78 publications

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“…Stellar feedback alters the mass density and dynamics of gas in star-forming environments (e.g., Lopez et al 2014;Menon et al 2021;Gallegos-Garcia et al 2020;Olivier et al 2021). Figure 4 shows normalized histograms of the gas density (left panel), velocity magnitude (middle panel), and momentum (right panel) for IsoRun (teal dashed lines) and AdiaRun (pink dotdashed lines) for the final snapshots at t = 0.2 Myr with the initial histograms over-plotted (gray solid lines).…”

Section: Gas Propertiesmentioning

confidence: 99%

“…Feedback from stellar winds may also sustain turbulence in molecular clouds (e.g., Arce et al 2011;Offner & Arce 2015;Li et al 2015;Feddersen et al 2018;Gallegos-Garcia et al 2020;Xu et al 2020b). As described in Histograms of the gas density (left), velocity (middle), and momentum (right) for the initial snapshot (gray lines) and final snapshots at t = 0.2 Myr for runs IsoRun (teal lines) and AdiaRun (pink lines).…”

Section: Driven Turbulencementioning

confidence: 99%

“…Previous work has explored how the stellar wind energy is transferred to the ISM (e.g., Weaver et al 1977;Harper-Clark & Murray 2009;Lopez et al 2011;Rogers & Pittard 2013;Rosen et al 2014;Fierlinger et al 2016;Gallegos-Garcia et al 2020;Lancaster et al 2021a). Much of this work has been motivated by the unexpectedly weak observed X-ray emission from star clusters that host many massive stars.…”

Section: Energy-conserving Vs Momentum-conserving Wind Bubblesmentioning

confidence: 99%

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Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough

Rosen,

Offner,

Foley

et al. 2021

Preprint

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Numerous spherical "shells" have been observed in young star-forming environments that host lowand intermediate-mass stars. These observations suggest that these shells may be produced by isotropic stellar wind feedback from young main-sequence stars. However, the driving mechanism for these shells remains uncertain because the momentum injected by winds is too low to explain their sizes and dynamics due to their low mass-loss rates. However, these studies neglect how the wind kinetic energy is transferred to the ISM and instead assume it is instantly lost via radiation, suggesting that these shells are momentum-driven. Intermediate-mass stars have fast (v w 1000 km/s) stellar winds and therefore the energy injected by winds should produce energy-driven adiabatic wind bubbles that are larger than momentum-driven wind bubbles. Here, we explore if energy-driven wind feedback can produce the observed shells by performing a series of 3D magneto-hydrodynamic simulations of wind feedback from intermediate-mass and high-mass stars that are placed in a magnetized, turbulent molecular cloud. We find that, for the high-mass stars modeled, energy-driven wind feedback produces ∼pc scale wind bubbles in molecular clouds that agree with the observed shell sizes but winds from intermediate-mass stars can not produce similar shells because of their lower mass-loss rates and velocities. Therefore, such shells must be driven by other feedback processes inherent to low-and intermediate-mass star formation.

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Section: Gas Propertiesmentioning

confidence: 99%

Section: Driven Turbulencementioning

confidence: 99%

Section: Energy-conserving Vs Momentum-conserving Wind Bubblesmentioning

confidence: 99%

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Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough

Rosen,

Offner,

Foley

et al. 2021

Preprint

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“…For the latter we take a fiducial value of 30% assuming equipartition between thermal, non thermal and turbulent energy in the superbubble (e.g. [24]).…”

Section: Transport Of Particles In Superbubblesmentioning

confidence: 99%

The cosmic ray content of superbubbles

Vieu¹,

Gabici²,

Tatischeff³

2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Although most massive stars are thought to live inside clusters giving rise to galactic-scale superbubbles, a complete model of cosmic ray production in these objects is still missing in the literature. We present an attempt to model particles acceleration in these systems including all the relevant physical processes. The acceleration mechanisms taking place in superbubbles differ from that occurring at isolated supernova remnants in several aspects. The presence of a magnetized shell is expected to efficiently confine the particles, which may therefore experience successive reaccelerations at supernovae shocks. The medium is also though to be highly turbulent, which hardens the particle spectra and makes shock acceleration nonlinear. Spectra are further shaped by losses, stellar winds, and the leakage of the interstellar cosmic rays through the superbubble shell. We discuss typical superbubble spectra and detail the time-dependent emission of these objects.

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“…Rogers & Pittard (2013) 2020) have all included stellar winds in star formation simulations, as well as numerous other works studying winds from single sources or in idealised settings (e.g. Gallegos-Garcia et al 2020) or on larger scales (e.g. Agertz et al 2013;Gatto et al 2017).…”

Section: Theory Of Stellar Wind Feedbackmentioning

confidence: 99%

Bottling the Champagne: Dynamics and Radiation Trapping of Wind-Driven Bubbles around Massive Stars

Geen,

de Koter

2021

Preprint

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In this paper we make predictions for the behaviour of wind bubbles around young massive stars using analytic theory. We do this in order to determine why there is a discrepancy between theoretical models that predict that winds should play a secondary role to photoionisation in the dynamics of H regions, and observations of young H regions that seem to suggest a driving role for winds. In particular, regions such as M42 in Orion have neutral hydrogen shells, suggesting that the ionising radiation is trapped closer to the star. We first derive formulae for wind bubble evolution in non-uniform density fields, focusing on singular isothermal sphere density fields with a power law index of -2. We find that a classical "Weaver"-like expansion velocity becomes constant in such a density distribution. We then calculate the structure of the photoionised shell around such wind bubbles, and determine at what point the mass in the shell cannot absorb all of the ionising photons emitted by the star, causing an "overflow" of ionising radiation. We also estimate perturbations from cooling, gravity, magnetic fields and instabilities, all of which we argue are secondary effects for the conditions studied here. Our wind-driven model provides a consistent explanation for the behaviour of M42 to within the errors given by observational studies. We find that in relatively denser molecular cloud environments around single young stellar sources, champagne flows are unlikely until the wind shell breaks up due to turbulence or clumping in the cloud.

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Winds in Star Clusters Drive Kolmogorov Turbulence

Cited by 23 publications

References 78 publications

Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough

Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough

The cosmic ray content of superbubbles

Bottling the Champagne: Dynamics and Radiation Trapping of Wind-Driven Bubbles around Massive Stars

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