Impact of Winds from Intermediate-Mass Stars on Molecular Cloud Structure and Turbulence

Abstract

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 characterized and the mass-loss rates inferred from the gas kinematics are several orders of magnitude greater than those predicted by atomic line-driven stellar wind models. We use magnetohydrodynamic simulations to model winds launching within turbulent molecular clouds and explore the impact of wind properties on cloud morphology and turbulence. We find that winds do not produce clear features in turbulent statistics such as the Fourier spectra of density and momentum but do impact the Fourier velocity spectrum. The density and velocity distribution functions, especially as probed by CO spectral lines, strongly indicate the presence and influence of winds. We show that stellar mass-loss rates for individual stars must be ${\dot{m}}_w\gtrsim 10^{-7}$ Msun yr${}^{-1}$, similar to those estimated from observations, to reproduce shell properties. Consequently, we conclude that B and A-type main sequence stars have mass-loss rates several orders of magnitude larger that those predicted by models or that young stars are more variable than expected due to magnetic activity or accretion.

20 pages, 13 figures. Accepted for publication in the Astrophysical Journal

References in corpus (16)

• Theory of Star Formation
• PLUTO: a Numerical Code for Computational Astrophysics
• The Statistics of Supersonic Isothermal Turbulence
• The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing
• The Effects of Radiative Transfer on Low-Mass Star Formation
• The COMPLETE Survey of Star-Forming Regions: Phase I Data
• On the interplay between star formation and feedback in galaxy formation simulations
• Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
• A Detailed Study of Feedback from a Massive Star
• IN-SYNC II: Virial Stars from Sub-Virial Cores -- The Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333
• Periodic accretion from a circumbinary disk in the young binary UZ Tau E
• The effect of stellar winds on the formation of a protocluster
• Jet Motion, Internal Working Surfaces, and Nested Shells in the Protostellar System HH 212
• The COMPLETE Nature of the Warm Dust Ring in Perseus
• Feedback from Winds and Supernovae in Massive Stellar Clusters - II. X-Ray Emission
• On X-ray pulsations in beta Cephei-type variables

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