Papers › The Co-Evolution of Stellar Wind-blown Bubbles and Photoionized Gas I: Physical...
The Co-Evolution of Stellar Wind-blown Bubbles and Photoionized Gas I: Physical Principles and a Semi-Analytic Model
Lachlan Lancaster, Jeong-Gyu Kim, Greg L. Bryan, Shyam H. Menon, Eve C. Ostriker, Chang-Goo Kim
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We propose a new framework for the simultaneous feedback of stellar winds and photo-ionizing radiation from massive stars, distinguishing the locations where forces are applied, and consequences for internal spatio-temporal evolution of the whole feedback bubble (FB). We quantify the relative dynamical importance of wind-blown bubbles (WBB) versus the photoionized region (PIR) by the ratio of the radius at which the WBB is in pressure equilibrium with the PIR, R_(eq), to the Str\"{o}mgren radius, R_(St). ζ≡R_(eq)/R_(St) quantifies the dynamical dominance of WBBs (ζ> 1) or the PIR (ζ< 1). We calculate ζ and find that, for momentum-driven winds, 0.1 ≲ζ≲1 for the star-forming regions in (i) typical Milky Way-like giant molecular clouds (GMCs), (ii) the most massive of individual OB stars, and (iii) dense, low-metallicity environments, relevant in the early universe. In this regime, both WBBs and the PIR are dynamically important to the expansion of the FB. We develop a semi-analytic Co-Evolution Model (CEM) that takes into account the spatial distribution of forces and the back reactions of both the WBB and PIR. In the ζ<1 regime where the CEM is most relevant, the model differs in the total FB momentum by up to 25% compared to naive predictions. In the weak-wind limit of ζ≪1, applicable to individual OB stars or low-mass clusters, the CEM has factors ≳2 differences in WBB properties. In a companion paper we compare these models to three-dimensional, turbulent hydro-dynamical simulations.
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