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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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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Journal ArticleDOI
When feedback fails: The scaling and saturation of star formation efficiency
Michael Y. Grudić,Philip F. Hopkins,Claude André Faucher-Giguère,Eliot Quataert,Norman Murray,Dušan Kereš +5 more
Abstract: We present a suite of 3D multiphysics MHD simulations following star formation in isolated turbulent molecular gas discs ranging from 5 to 500 parsecs in radius. These simulations are designed to survey the range of surface densities between those typical of Milky Way giant molecular clouds (GMCs) (∼10^2M⊙pc^(−2)) and extreme ultraluminous infrared galaxy environments (∼10^4M⊙pc^(−2)) so as to map out the scaling of the cloud-scale star formation efficiency (SFE) between these two regimes. The simulations include prescriptions for supernova, stellar wind, and radiative feedback, which we find to be essential in determining both the instantaneous per-freefall (e_(ff)) and integrated (e_(int)) star formation efficiencies. In all simulations, the gas discs form stars until a critical stellar surface density has been reached and the remaining gas is blown out by stellar feedback. We find that surface density is a good predictor of e_(int), as suggested by analytic force balance arguments from previous works. SFE eventually saturates to ∼1 at high surface density. We also find a proportional relationship between e_(ff) and e_(int), implying that star formation is feedback-moderated even over very short time-scales in isolated clouds. These results have implications for star formation in galactic discs, the nature and fate of nuclear starbursts, and the formation of bound star clusters. The scaling of e_(ff) with surface density is not consistent with the notion that e_(ff) is always ∼ 1 per cent on the scale of GMCs, but our predictions recover the ∼ 1 per cent value for GMC parameters similar to those found in spiral galaxies, including our own.
Journal ArticleDOI
What is a globular cluster? An observational perspective
Raffaele Gratton,Angela Bragaglia,Eugenio Carretta,Valentina D'Orazi,Valentina D'Orazi,Sara Lucatello,Sara Lucatello,Antonio Sollima +7 more
TL;DR: In this paper, the authors focus on the main observational features of clusters in the Milky Way and its satellites, and find that most of the observational facts related to the chemical evolution in globular clusters are described as being primarily a function of the initial mass of the clusters, tuned by further dependence on the metallicity, which likely determines the possibility of independent chemical evolution of the fragments or satellites, where the clusters form.
Journal ArticleDOI
Observational evidence of dynamic star formation rate in milky way giant molecular clouds
TL;DR: In this article, the authors cross-correlate 5469 giant molecular clouds (GMCs) from a new all-sky catalog with 256 star forming complexes (SFCs) to build a sample of 191 SFC-GMC complexes.
Journal ArticleDOI
Simulations of magnetized multiphase galactic disc regulated by supernovae explosions
TL;DR: In this article, the role of supernovae feedback and magnetic field on the star formation and the structure of the Galactic disc is investigated, and it is shown that the supernova feedback has a drastic influence on the galactic evolution.
Journal ArticleDOI
One-dimensional dynamical models of the carina nebula bubble
E. Harper-Clark,N. Murray +1 more
TL;DR: In this article, the authors modify the Castor et al. theory to take into account lower stellar wind mass-loss rates, radiation pressure, gravity, and escape of or energy loss from the hot shocked gas.