Winds in Star Clusters Drive Kolmogorov Turbulence

@article{GallegosGarcia2020WindsIS,
  title={Winds in Star Clusters Drive Kolmogorov Turbulence},
  author={Monica Gallegos-Garcia and Blakesley Burkhart and Anna L. Rosen and J. P. Naiman and Enrico Ramirez-Ruiz},
  journal={The Astrophysical Journal Letters},
  year={2020},
  volume={899}
}
Intermediate and massive stars drive fast and powerful isotropic winds that interact with the winds of nearby stars in star clusters and the surrounding interstellar medium (ISM). Wind–ISM collisions generate astrospheres around these stars that contain hot T ∼ 107 K gas that adiabatically expands. As individual bubbles expand and collide they become unstable, potentially driving turbulence in star clusters. In this Letter we use hydrodynamic simulations to model a densely populated young star… 

Diagnosing Turbulence in the Neutral and Molecular Interstellar Medium of Galaxies

  • B. Burkhart
  • Physics
    Publications of the Astronomical Society of the Pacific
  • 2021
Magnetohydrodynamic (MHD) turbulence is a crucial component of the current paradigms of star formation, dynamo theory, particle transport, magnetic reconnection, and evolution of structure in the

Efficient early stellar feedback can suppress galactic outflows by reducing supernova clustering

We present a novel set of stellar feedback models, implemented in the moving-mesh code arepo, designed for galaxy formation simulations with near-parsec (or better) resolution. These include

The cosmic ray content of superbubbles

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

Classification of Magnetohydrodynamic Simulations Using Wavelet Scattering Transforms

The complex interplay of magnetohydrodynamics, gravity, and supersonic turbulence in the interstellar medium (ISM) introduces a non-Gaussian structure that can complicate a comparison between theory

Quantitative analysis of production of turbulent kinetic energy by using catastrophe method for the whole process of turbulence formation

The whole process of turbulence formation was quantitatively studied by the catastrophe method. The change law of the production of turbulent kinetic energy and its spectral distribution with the

Can superbubbles accelerate ultrahigh energy protons?

We critically assess limits on the maximum energy of protons accelerated within superbubbles around massive stellar clusters, considering a number of different scenarios. In particular, we derive

Studying Interstellar Turbulence Driving Scales Using the Bispectrum

We demonstrate the utility of the bispectrum, the Fourier three-point correlation function, for studying driving scales of magnetohydrodynamic (MHD) turbulence in the interstellar medium. We

The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density Probability Distribution Function in Turbulent Star-forming Clouds

Using a suite of 3D hydrodynamical simulations of star-forming molecular clouds, we investigate how the density probability distribution function (PDF) changes when including gravity, turbulence,

References

SHOWING 1-10 OF 83 REFERENCES

Gone with the wind: Where is the missing stellar wind energy from massive star clusters?

Star clusters larger than $\sim 10^{3}$ $M_\odot$ contain multiple hot stars that launch fast stellar winds. The integrated kinetic energy carried by these winds is comparable to that delivered by

IMPACT OF WINDS FROM INTERMEDIATE-MASS STARS ON MOLECULAR CLOUD STRUCTURE AND TURBULENCE

Observations of nearby molecular clouds detect “shells,” which are likely caused by winds from young main sequence stars. However, the progenitors of these observed features are not well

Clustered supernovae drive powerful galactic winds after superbubble breakout

We use three-dimensional hydrodynamic simulations of vertically stratified patches of galactic discs to study how the spatio-temporal clustering of supernovae (SNe) enhances the power of galactic

MOLECULAR RINGS AROUND INTERSTELLAR BUBBLES AND THE THICKNESS OF STAR-FORMING CLOUDS

The winds and radiation from massive stars clear out large cavities in the interstellar medium. These bubbles, as they have been called, impact their surrounding molecular clouds and may influence

Moving-mesh Simulations of Star-forming Cores in Magneto-gravo-turbulence

Star formation in our Galaxy occurs in molecular clouds that are self-gravitating, highly turbulent, and magnetized. We study the conditions under which cloud cores inherit large-scale magnetic field

Runaway stars as cosmic ray injectors inside molecular clouds

Giant molecular clouds (GMCs) are a new population of gamma-ray sources, being the target of cosmic rays (CRs) – locally accelerated or not –. These clouds host very young stellar clusters where

Stellar wind retention and expulsion in massive star clusters

Mass and energy injection throughout the lifetime of a star cluster contributes to the gas reservoir available for subsequent episodes of star formation and the feedback energy budget responsible for

Detecting stellar-wind bubbles through infrared arcs in H ii regions

Mid-infrared arcs of dust emission are often seen near ionizing stars within HII regions. A possible explanations for these arcs is that they could show the outer edges of asymmetric stellar wind

Numerical simulations of supernova remnants in turbulent molecular clouds

Core-collapse supernova (SN) explosions may occur in the highly inhomogeneous molecular clouds (MCs) in which their progenitors were born. We perform a series of 3-dimensional hydrodynamic

The Hot, Diffuse Gas in a Dense Cluster of Massive Stars

We present an analytic model describing the "cluster wind" flow that results from the multiple interaction of the stellar winds produced by the stars of a dense cluster of massive stars. The analytic
...