The formation of massive stellar clusters in converging galactic flows with photoionization

Dobbs, Clare; Bending, Thomas; Pettitt, Alex R.; Bate, Matthew R.

doi:10.1093/mnras/stab3036

Cited by 24 publications

(42 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Motivated by recent numerical and observational findings (e.g., Kim et al 2018b;Tsuge et al 2021), we simulated the formation of a massive compact cluster via the collision of two GMCs, each weighing 3.6 × 10 5 M e , using RHD simulations. In particular, we focused on the impact of radiation feedback on the formation process of GC candidates and found that it can play an important role in determining the star formation histories, stellar masses, and metallicity distributions (see also Dobbs et al 2022). Our results are summarized as follows.…”

Section: Discussionmentioning

confidence: 92%

“…We present one of the first studies that attempt to understand the impact of radiation feedback on the formation of massive compact clusters using RHD (see also Dobbs et al 2022). However, several caveats should be considered when interpreting our results.…”

Section: Caveatsmentioning

confidence: 94%

“…Recently, Dobbs et al (2022) reported the impact of photoionization in a dense region of a spiral galaxy with converging flows. More specifically, they simulated cluster formation in strongly and moderately converging regions along a spiral arm in the disks of galaxies similar to the Milky Way.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

Han

Kimm

Katz

et al. 2022

ApJ

View full text Add to dashboard Cite

To understand the impact of radiation feedback during the formation of a globular cluster (GC), we simulate a head-on collision of two turbulent giant molecular clouds (GMCs). A series of idealized radiation-hydrodynamic simulations is performed, with and without stellar radiation or Type II supernovae. We find that a gravitationally bound, compact star cluster of mass M GC ∼ 105 M ⊙ forms within ≈3 Myr when two GMCs with mass M GMC = 3.6 × 105 M ⊙ collide. The GC candidate does not form during a single collapsing event but emerges due to the mergers of local dense gas clumps and gas accretion. The momentum transfer due to the absorption of the ionizing radiation is the dominant feedback process that suppresses the gas collapse, and photoionization becomes efficient once a sufficient number of stars form. The cluster mass is larger by a factor of ∼2 when the radiation feedback is neglected, and the difference is slightly more pronounced (16%) when extreme Lyα feedback is considered in the fiducial run. In the simulations with radiation feedback, supernovae explode after the star-forming clouds are dispersed, and their metal ejecta are not instantaneously recycled to form stars.

show abstract

Section: Discussionmentioning

confidence: 92%

Section: Caveatsmentioning

confidence: 94%

See 1 more Smart Citation

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

Han

Kimm

Katz

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

Section: Introductionmentioning

confidence: 99%

“…Simulations can take into account of surrounding gas by resimulating, or zooming in on small sections of whole galaxy simulations (Van Loo et al 2013;Smilgys & Bonnell 2017;Bending et al 2020;Ali 2021;Rieder et al 2022;Smith et al 2020;Dobbs et al 2022). Dobbs et al (2022) showed that colliding flows on larger scales are significant in determining the final cluster mass, partly because they lead to more mergers between clusters. Generally, simulations show that at least for the formation of more massive clusters, cluster formation is hierarchical and mergers are frequent (Bonnell et al 2003;Smilgys & Bonnell 2017;Fujii & Portegies Zwart 2015;Fujii et al 2021;Guszejnov et al 2022;Dobbs et al 2022).…”

Section: Introductionmentioning

confidence: 99%

The formation of clusters and OB associations in different density spiral arm environments

Dobbs

Bending

Pettitt

et al. 2022

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present simulations of the formation and evolution of clusters in spiral arms. The simulations follow two different spiral arm regions, and the total gas mass is varied to produce a range of different mass clusters. We find that including photoionizing feedback produces the observed cluster mass radius relation, increasing the radii of clusters compared to without feedback. Supernovae have little impact on cluster properties. We find that in our high density, high gas mass simulations, star formation is less affected by feedback, as star formation occurs rapidly before feedback has much impact. In our lowest gas density simulation, the resulting clusters are completely different (e.g. the number of clusters and their masses) to the case with no feedback. The star formation rate is also significantly suppressed. The fraction of stars in clusters in this model decreases with time flattening at about 20 per cent. In our lowest gas simulation model, we see the formation of a star forming group with properties similar to an OB association, in particular similar to Orion Ia. We suggest that low densities, and stronger initial dynamics are conducive to forming associations rather than clusters. In all models cluster formation is complex with clusters merging and splitting. The most massive clusters which form have tended to undergo more mergers.

show abstract

Universal gravity-driven isothermal turbulence cascade in disk galaxies

Fensch¹,

F.²,

Brucy³

et al. 2023

A&A

View full text Add to dashboard Cite

While interstellar gas is known to be supersonically turbulent, the injection processes of this turbulence are still unclear. Many studies suggest a dominant role of gravitational instabilities. However, their effect on galaxy morphology and large-scale dynamics varies across cosmic times, in particular, due to the evolution of the gas fraction of galaxies. In this paper, we propose numerical simulations to follow the isothermal turbulent cascade of purely gravitationally driven turbulence from its injection scale down to 0.095 pc for a gas-poor spiral disk and a gas-rich clumpy disk. For this purpose, and to lift the memory-footprint technical lock of sufficiently resolving the interstellar medium of a galaxy, we developed an encapsulated zoom method that allows us to self-consistently probe the self-generated turbulence cascade over three orders of magnitude on spatial scales. We followed this cascade for 10 Myr. We find that the turbulent cascade follows the same scaling laws in both setups. Namely, in both cases, the turbulence is close to equipartition between its compressive and solenoidal modes, the velocity power spectrum follows the Burgers scaling, and the density power spectrum is rather shallow, with a power-law slope of −0.7. Last, gravitationally bound substructures follow a mass distribution with a −1.8 slope, similar to that of CO clumps. These simulations thus suggest that gravity-driven isothermal turbulent cascades are universal in disk galaxies across cosmic time.

show abstract

The formation of massive stellar clusters in converging galactic flows with photoionization

Cited by 24 publications

References 76 publications

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

Impact of Radiation Feedback on the Formation of Globular Cluster Candidates during Cloud–Cloud Collisions

The formation of clusters and OB associations in different density spiral arm environments

Universal gravity-driven isothermal turbulence cascade in disk galaxies

Contact Info

Product

Resources

About