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| Main Authors: | , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2505.22730 |
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| _version_ | 1866913864881274880 |
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| author | Lancaster, Lachlan Kim, Jeong-Gyu Bryan, Greg L. Menon, Shyam H. Ostriker, Eve C. Kim, Chang-Goo |
| author_facet | Lancaster, Lachlan Kim, Jeong-Gyu Bryan, Greg L. Menon, Shyam H. Ostriker, Eve C. Kim, Chang-Goo |
| contents | 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, $R_{\rm eq}$, to the Strömgren radius, $R_{\rm St}$. $ζ\equiv R_{\rm eq}/R_{\rm St}$ quantifies the dynamical dominance of WBBs ($ζ> 1$) or the PIR ($ζ< 1$). We calculate $ζ$ and find that, for momentum-driven winds, $0.1 \lesssim ζ\lesssim 1$ 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 $ζ\ll 1$, applicable to individual OB stars or low-mass clusters, the CEM has factors $\gtrsim 2$ differences in WBB properties. In a companion paper we compare these models to three-dimensional, turbulent hydro-dynamical simulations. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_22730 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Co-Evolution of Stellar Wind-blown Bubbles and Photoionized Gas I: Physical Principles and a Semi-Analytic Model Lancaster, Lachlan Kim, Jeong-Gyu Bryan, Greg L. Menon, Shyam H. Ostriker, Eve C. Kim, Chang-Goo Astrophysics of Galaxies 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, $R_{\rm eq}$, to the Strömgren radius, $R_{\rm St}$. $ζ\equiv R_{\rm eq}/R_{\rm St}$ quantifies the dynamical dominance of WBBs ($ζ> 1$) or the PIR ($ζ< 1$). We calculate $ζ$ and find that, for momentum-driven winds, $0.1 \lesssim ζ\lesssim 1$ 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 $ζ\ll 1$, applicable to individual OB stars or low-mass clusters, the CEM has factors $\gtrsim 2$ differences in WBB properties. In a companion paper we compare these models to three-dimensional, turbulent hydro-dynamical simulations. |
| title | The Co-Evolution of Stellar Wind-blown Bubbles and Photoionized Gas I: Physical Principles and a Semi-Analytic Model |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2505.22730 |