Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds. I. Fractal Theory and Application to Star-forming Clouds
TLDR
In this article, the authors developed a theory for the evolution of bubbles driven by the collective winds from star clusters early in their lifetimes, which involves interaction with the turbulent, dense interstellar medium of the surrounding natal molecular cloud.Abstract:
Winds from massive stars have velocities of 1000 km/s or more, and produce hot, high pressure gas when they shock. We develop a theory for the evolution of bubbles driven by the collective winds from star clusters early in their lifetimes, which involves interaction with the turbulent, dense interstellar medium of the surrounding natal molecular cloud. A key feature is the fractal nature of the hot bubble's surface. The large area of this interface with surrounding denser gas strongly enhances energy losses from the hot interior, enabled by turbulent mixing and subsequent cooling at temperatures T = 10^4-10^5 K where radiation is maximally efficient. Due to the extreme cooling, the bubble radius scales differently (R ~ t^1/2) from the classical Weaver77 solution, and has expansion velocity and momentum lower by factors of 10-10^2 at given R, with pressure lower by factors of 10^2 - 10^3. Our theory explains the weak X-ray emission and low shell expansion velocities of observed sources. We discuss further implications of our theory for observations of the hot bubbles and cooled expanding shells created by stellar winds, and for predictions of feedback-regulated star formation in a range of environments. In a companion paper, we validate our theory with a suite of hydrodynamic simulations.read more
Citations
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Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds. II. Validation of Theory with Hydrodynamic Simulations
TL;DR: In this paper, the authors developed a theory for the evolution of stellar wind driven bubbles in dense, turbulent clouds and validated their theory with three-dimensional, hydrodynamic simulations, showing that extreme cooling is not only possible, but is generic to star formation in turbulent clouds over more than three orders of magnitude in density.
Journal ArticleDOI
Photodissociation and X-Ray-Dominated Regions
TL;DR: The radiation from stars and active galactic nuclei (AGNs) creates photodissociation regions (PDRs) and X-ray-dominated regions (XDRs), where the chemistry or heating are dominated by far-ultraviolet (FUV) radiation or Xray radiation, respectively as discussed by the authors .
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Comparing the pre-SNe feedback and environmental pressures for 6000 H ii regions across 19 nearby spiral galaxies
Ashley T. Barnes,Simon C. O. Glover,Kathryn Kreckel,Eve C. Ostriker,Frank Bigiel,Francesco Belfiore,Ivana Bešlić,Guillermo A. Blanc,Guillermo A. Blanc,Mélanie Chevance,Daniel A. Dale,Oleg V. Egorov,Oleg V. Egorov,Cosima Eibensteiner,Eric Emsellem,Kathryn Grasha,Brent Groves,Ralf S. Klessen,J. M. D. Kruijssen,Adam K. Leroy,S. N. Longmore,Laura A. Lopez,R. McElroy,Sharon Meidt,Eric J. Murphy,Erik Rosolowsky,Takashi Saito,F. Santoro,Eva Schinnerer,Andreas Schruba,Jiayi Sun,Elizabeth J. Watkins,Thomas G. Williams +32 more
TL;DR: In this paper, the authors assess the feedback mechanisms acting within a sample of 5810 HII regions identified from the PHANGS-MUSE survey of 19 nearby ($ 1), yet there is a small sample of compact H II regions with $P_\mathrm{tot,max}/P_ \mathm{de} < 1$ ($sim$1% of the sample).
Journal ArticleDOI
Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Eve C. Ostriker,Changgon Kim +1 more
TL;DR: In this article , a pressure-regulated, feedback-modulated (PRFM) theory of the star-forming ISM was proposed, leading to a prediction that the star formation rate per unit area, ΣSFR, will scale nearly linearly with ISM weight.
Journal ArticleDOI
Outflows from Super Star Clusters in the Central Starburst of NGC253
Rebecca C. Levy,Alberto D. Bolatto,Adam K. Leroy,K. L. Emig,Mark Gorski,Nico Krieger,Laura Lenkić,David S. Meier,Elisabeth A. C. Mills,Juergen Ott,Erik Rosolowsky,Elizabeth Tarantino,Sylvain Veilleux,Fabian Walter,Axel Weiss,Martin Zwaan +15 more
TL;DR: In this article, the authors used ALMA data at 350 GHz with 28 milliarcsecond (0.5 pc) resolution to detect blueshifted absorption and redshifted emission (P-Cygni profiles) towards three super star clusters in multiple lines, including CS 7$-$6 and H$−13$CN 4$-$3, which represents direct evidence for previously unobserved outflows.
References
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What Drives the Expansion of Giant HII Regions?: A Study of Stellar Feedback in 30 Doradus
TL;DR: In this article, high-resolution, multi-wavelengh images (radio, infrared, optical, and X-ray) were used to map these pressures as a function of position and found that radiation pressure dominates within 75 pc of the central star cluster, R136, while the HII gas pressure dominates at larger radii.
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Superbubbles in the multiphase ism and the loading of galactic winds
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