Stellar feedback and triggered star formation in the prototypical bubble RCW 120

Luisi, Matteo; Anderson, L. D.; Schneider, N.; Simon, R.; Kabanovic, S.; Güsten, R.; Zavagno, A.; Broos, P. S.; Buchbender, C.; Guevara, C.; Jacobs, K.; Justen, M.; Klein, Bernd; Linville, Dylan; Röllig, M.; Russeil, D.; Stützki, J.; Tiwari, M.; Townsley, Leisa K.; Tielens, A. G. G. M.

doi:10.1126/sciadv.abe9511

Cited by 40 publications

(37 citation statements)

References 76 publications

(79 reference statements)

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“…An analysis of the Orion Veil [C II], associated with the M42 H II region (Pabst et al 2019(Pabst et al , 2020 and seen in the Orion map (Figure 11 to the south west) find the neutral shell is expanding at 13 km s −1 , and, along with estimates of the various feedback pressures using observations of Hα, CO, and X-rays, is interpreted as a consequence of a wind-blown bubble as discussed in Section 6. A similar result was found analyzing the [C II] emission in RCW 120 (Luisi et al 2021). The bubbles in the M43 and NGC 1977 regions to the north of M42 are powered by early B stars, with weak winds, and are found instead to be dominated by the thermal expansion of the H II region (Pabst et al 2020).…”

Section: Preparation)supporting

confidence: 81%

Photodissociation and X-Ray Dominated Regions

Wolfire¹,

Vallini²,

Chevance³

2022

Preprint

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The radiation from stars and active galactic nuclei (AGN) creates photodissociation regions (PDRs) and X-ray dominated regions (XDRs), where the chemistry or heating are dominated by far-ultraviolet (FUV) radiation or X-ray radiation, respectively. PDRs include a wide range of environments from the diffuse interstellar medium to dense star-forming regions. XDRs are found in the center of galaxies hosting AGN, in protostellar disks, and in the vicinity of X-ray binaries. In this review, we describe the dominant thermal, chemical, and radiation transfer processes in PDRs and XDRs, as well as a brief description of models and their use to analyze observations. We then present recent results from Milky Way, nearby extragalactic, and high-redshift observations. Several important results are:

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Section: Preparation)supporting

confidence: 81%

Photodissociation and X-Ray Dominated Regions

Wolfire¹,

Vallini²,

Chevance³

2022

Preprint

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“…They found that none of the following factors: photo-destruction by ultraviolet photons, radiation pressure and overall expansion of H ii regions can explain all the observed IR features alone. Recent observations of H ii regions by SOFIA telescope revealed the importance of stellar wind in dynamics of ionised gas around O-type stars, see e. g. Pabst et al (2019), Luisi et al (2021). Following these results, we numerically explore the influence of the wind on dust dynamics and simulate mid and far-IR emission from H ii regions.…”

Section: Introductionmentioning

confidence: 85%

Infrared appearance of wind-blown bubbles around young massive stars

Kirsanova¹,

Pavlyuchenkov²

2022

Preprint

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Thousands of ring-like bubbles appear on infrared images of the Galaxy plane. Most of these infrared bubbles form during expansion of H ii regions around massive stars. However, the physical effects that determine their morphology are still under debate. Namely, the absence of the infrared emission toward the centres of the bubbles can be explained by pushing the dust grains by stellar radiation pressure. At the same time, small graphite grains and PAHs are not strongly affected by the radiation pressure and must be removed by another process. Stellar ultraviolet emission can destroy the smallest PAHs but the photodestruction is ineffective for the large PAHs. Meanwhile, the stellar wind can evacuate all types of grains from H ii regions. In the frame of our chemo-dynamical model we vary parameters of the stellar wind and illustrate their influence on the morphology and synthetic infrared images of the bubbles.

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“…Stellar wind pushes out surrounding gas (e.g., Dale et al 2014;Decataldo et al 2020;Geen et al 2021;Rosen et al 2021), and heats up the gas to ( 10 5 K) via the shock (e.g., Lancaster et al 2021a,b). Indeed, X-ray emission is observed from the region inside the expanding shell (Luisi et al 2021), which is likely to be induced by the stellar wind. We will include these effects in future works.…”

Section: Discussionmentioning

confidence: 99%

Far and extreme UV radiation feedback in molecular clouds and its influence on the mass and size of star clusters

Fukushima,

Yajima

2022

Preprint

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We study the formation of star clusters in molecular clouds by performing three-dimensional radiation hydrodynamics simulations with far ultraviolet (FUV; 6 eV ℎ𝜈 13.6 eV) and extreme ultraviolet (EUV; ℎ𝜈 13.6 eV) radiative feedback. We find that the FUV feedback significantly suppresses the star formation in diffuse clouds with the initial surface densities of Σ cl 50 M pc −2 . In the cases of clouds with Σ cl ∼ 100 − 200 M pc −2 , the EUV feedback plays a main role and decrease the star formation efficiencies less than 0.3. We show that thermal pressure from PDRs or H regions disrupts the clouds and makes the size of the star clusters larger. Consequently, the clouds with the mass 𝑀 cl 10 5 M and the surface density Σ cl 200 M pc −2 remain the star clusters with the stellar densities of ∼ 100 M pc −3 that nicely match the observed open clusters in the Milky Way. If the molecular clouds are massive (𝑀 cl 10 5 M ) and compact (Σ 400 M pc −2 ), the radiative feedback is not effective and they form massive dense cluster with the stellar densities of ∼ 10 4 M pc −3 like observed globular clusters or young massive star clusters. Thus, we suggest that the radiative feedback and the initial conditions of molecular clouds are key factors inducing the variety of the observed star clusters.

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Stellar feedback and triggered star formation in the prototypical bubble RCW 120

Cited by 40 publications

References 76 publications

Photodissociation and X-Ray Dominated Regions

Photodissociation and X-Ray Dominated Regions

Infrared appearance of wind-blown bubbles around young massive stars

Far and extreme UV radiation feedback in molecular clouds and its influence on the mass and size of star clusters

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