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
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Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
TL;DR: In this article , an Eulerian hydrodynamic code Athena++ was used to find universal scaling relations for the time evolution of momentum and radius for a superbubble, when the momentum and time are scaled by those at the shell-formation time.
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Far and extreme UV radiation feedback in molecular clouds and its influence on the mass and size of star clusters
Y Fukushima,Hidenobu Yajima +1 more
TL;DR: In this article , the formation of star clusters in molecular clouds was studied by performing three-dimensional radiation hydrodynamics simulations with far ultraviolet (FUV; 6 eV≦hν≦13.6 eV) radiative feedback.
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Outflows from Super Star Clusters in the Central Starburst of NGC 253
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,Jürgen Ott,Erik Rosolowsky,Elizabeth Tarantino,Sylvain Veilleux,Fabian Walter,A. Weiß,Martin Zwaan +15 more
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Infrared Radiation Feedback Does Not Regulate Star Cluster Formation
TL;DR: In this article , a 3D radiation-hydrodynamical (RHD) simulation of star cluster formation and evolution in massive, self-gravitating clouds, whose dust columns are optically thick to infrared (IR) photons is presented.
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Filamentary structures of ionized gas in Cygnus X
K. L. Emig,Glenn J. White,P. Salas,Ramsey L. Karim,R. J. van Weeren,P. Teuben,Annie Zavagno,Po-Jian Chiu,Marijke Haverkorn,J. B. R. Oonk,Emanuela Orru,I.M. Polderman,W. Reich,Huub Rottgering,Alexander G. G. M. Tielens +14 more
TL;DR: In this paper , the authors used DisPerSE and FilChaP to identify filamentary structures and characterize their radial (EM) pro�les in the Cygnus X region.
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