The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models
In a companion paper (Paper I), we presented a coevolution model (CEM) in which to consider the evolution of feedback bubbles driven by massive stars through both stellar winds and ionizing radiation, outlining when either of these effects is dominant and providing a model for how they evolve togeth...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ade66c |
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| author | Lachlan Lancaster Chang-Goo Kim Jeong-Gyu Kim Eve C. Ostriker Greg L. Bryan |
| author_facet | Lachlan Lancaster Chang-Goo Kim Jeong-Gyu Kim Eve C. Ostriker Greg L. Bryan |
| author_sort | Lachlan Lancaster |
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| description | In a companion paper (Paper I), we presented a coevolution model (CEM) in which to consider the evolution of feedback bubbles driven by massive stars through both stellar winds and ionizing radiation, outlining when either of these effects is dominant and providing a model for how they evolve together. Here we present results from 3D radiation magnetohydrodynamical simulations of this scenario for parameters typical of massive star-forming clouds in the Milky Way: precisely the regime where we expect both feedback mechanisms to matter. While we find that the CEM agrees with the simulations to within 25% for key parameters and modestly outperforms previous idealized models, disagreements remain. We show that these deviations originate mainly from the CEM’s lack of (i) background inhomogeneity caused by turbulence and (ii) time-variable momentum enhancements in the wind-blown bubble (WBB). Additionally, we find that photoionized gas acts similarly to magnetic fields by decreasing the WBB’s surface area. This causes a decrease in the amount of cooling at the WBB’s interface, resulting in an enhanced WBB dynamical impact. |
| format | Article |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-3f9bad55c1b646e3816fa7b64a4cdeea2025-08-20T03:38:06ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198914310.3847/1538-4357/ade66cThe Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic ModelsLachlan Lancaster0https://orcid.org/0000-0002-0041-4356Chang-Goo Kim1https://orcid.org/0000-0003-2896-3725Jeong-Gyu Kim2https://orcid.org/0000-0001-6228-8634Eve C. Ostriker3https://orcid.org/0000-0002-0509-9113Greg L. Bryan4https://orcid.org/0000-0003-2630-9228Department of Astronomy, Columbia University , 550 W 120th Street, New York, NY 10025, USA; Center for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USADepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USAKorea Institute of Advanced Study , 85 Hoegi-ro, Dongdaemun-gu, Seoul 02455, Republic of Korea; Division of Science, National Astronomical Observatory of Japan , Mitaka, Tokyo 181-0015, JapanDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA; Institute for Advanced Study , 1 Einstein Drive, Princeton, NJ 08540, USADepartment of Astronomy, Columbia University , 550 W 120th Street, New York, NY 10025, USA; Center for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USAIn a companion paper (Paper I), we presented a coevolution model (CEM) in which to consider the evolution of feedback bubbles driven by massive stars through both stellar winds and ionizing radiation, outlining when either of these effects is dominant and providing a model for how they evolve together. Here we present results from 3D radiation magnetohydrodynamical simulations of this scenario for parameters typical of massive star-forming clouds in the Milky Way: precisely the regime where we expect both feedback mechanisms to matter. While we find that the CEM agrees with the simulations to within 25% for key parameters and modestly outperforms previous idealized models, disagreements remain. We show that these deviations originate mainly from the CEM’s lack of (i) background inhomogeneity caused by turbulence and (ii) time-variable momentum enhancements in the wind-blown bubble (WBB). Additionally, we find that photoionized gas acts similarly to magnetic fields by decreasing the WBB’s surface area. This causes a decrease in the amount of cooling at the WBB’s interface, resulting in an enhanced WBB dynamical impact.https://doi.org/10.3847/1538-4357/ade66cMagnetohydrodynamical simulationsRadiative transfer simulationsH II regionsStellar wind bubblesInterstellar medium |
| spellingShingle | Lachlan Lancaster Chang-Goo Kim Jeong-Gyu Kim Eve C. Ostriker Greg L. Bryan The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models The Astrophysical Journal Magnetohydrodynamical simulations Radiative transfer simulations H II regions Stellar wind bubbles Interstellar medium |
| title | The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models |
| title_full | The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models |
| title_fullStr | The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models |
| title_full_unstemmed | The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models |
| title_short | The Coevolution of Stellar Wind-blown Bubbles and Photoionized Gas. II. 3D RMHD Simulations and Tests of Semianalytic Models |
| title_sort | coevolution of stellar wind blown bubbles and photoionized gas ii 3d rmhd simulations and tests of semianalytic models |
| topic | Magnetohydrodynamical simulations Radiative transfer simulations H II regions Stellar wind bubbles Interstellar medium |
| url | https://doi.org/10.3847/1538-4357/ade66c |
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