The formation of young massive clusters by colliding flows

Dobbs, Clare; Liow, Kong You; Rieder, Steven

doi:10.1093/mnrasl/slaa072

Cited by 41 publications

(38 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Furthermore whilst the previous numerical studies do not find large global changes, have found that particularly massive GMCs can form in the presence of stronger, or tidally induced spiral arms (Dobbs et al 2011;Pettitt et al 2018) compared to weaker or flocculent spiral arms. Small scale models of colliding flows also find that strongly converging flows lead to massive clusters (Dobbs et al 2020;. Such conditions would more likely occur in galaxies with stronger spiral arms, or locations in galaxies where localised strongly converging flows occur (Eden et al 2012;Motte et al 2014).…”

Section: Introductionmentioning

confidence: 95%

See 1 more Smart Citation

The formation and early evolution of embedded star clusters in spiral galaxies

Rieder

Dobbs

Bending

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present Ekster, a new method for simulating star clusters from birth in a live galaxy simulation that combines the smoothed-particle hydrodynamics (SPH) method Phantom with the N-body method PeTar. With Ekster, it becomes possible to simulate individual stars in a simulation with only moderately high resolution for the gas, allowing us to study whole sections of a galaxy rather than be restricted to individual clouds. We use this method to simulate star and star cluster formation in spiral arms, investigating massive GMCs and spiral arm regions with lower mass clouds, from two galaxy models with different spiral potentials. After selecting these regions from pre-run galaxy simulations, we re-sample the particles to obtain a higher resolution. We then re-simulate these regions for 3 Myr to study where and how star clusters form. We analyse the early evolution of the embedded star clusters in these regions. We find that the massive GMC regions, which are more common with stronger spiral arms, form more massive clusters than the sections of spiral arms containing lower mass clouds. Clusters form both by accreting gas and by merging with other proto-clusters, the latter happening more frequently in the denser GMC regions.

show abstract

Section: Introductionmentioning

confidence: 95%

“…Since changing galactic dynamics can have a major impact on the formation of stars (e.g. due to colliding flows, Inutsuka et al 2015;Dobbs et al 2020), this is not ideal.…”

Section: Introductionmentioning

confidence: 99%

The formation and early evolution of embedded star clusters in spiral galaxies

Rieder

Dobbs

Bending

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…from our previous work (Dobbs et al 2020; hold. Even in the case where the impact of the magnetic field is strongest, whilst we see a delay in star formation, we then see star formation rates which are similar to the other models.…”

Section: Discussionmentioning

confidence: 66%

“…This velocity is chosen so that the collision has a significant effect on star formation, i.e. the collision enhances the star formation rate above that which would occur for isolated clouds (Dobbs et al 2020), but is still consistent with the highest velocities observed for colliding streams in the Milky Way (Motte et al 2014;Fukui et al 2015Fukui et al , 2018. In we show results with different cloud dimensions and collision velocities, but here we focus on varying the magnetic field strength and orientation.…”

Section: Details Of Simulationsmentioning

confidence: 87%

See 1 more Smart Citation

The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds

Dobbs

Wurster

2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We have performed Smoothed Particle Magneto-Hydrodynamics (SPMHD) calculations of colliding clouds to investigate the formation of massive stellar clusters, adopting a timestep criterion to prevent large divergence errors. We find that magnetic fields do not impede the formation of young massive clusters (YMCs), and the development of high star formation rates, although we do see a strong dependence of our results on the direction of the magnetic field. If the field is initially perpendicular to the collision, and sufficiently strong, we find that star formation is delayed, and the morphology of the resulting clusters is significantly altered. We relate this to the large amplification of the field with this initial orientation. We also see that filaments formed with this configuration are less dense. When the field is parallel to the collision, there is much less amplification of the field, dense filaments form, and the formation of clusters is similar to the purely hydrodynamical case. Our simulations reproduce the observed tendency for magnetic fields to be aligned perpendicularly to dense filaments, and parallel to low density filaments. Overall our results are in broad agreement with past work in this area using grid codes.

show abstract

Ionized carbon as a tracer of the assembly of interstellar clouds

et al. 2023

View full text Add to dashboard Cite

Molecular hydrogen clouds are a key component of the interstellar medium because they are the birthplaces for stars. They are embedded in atomic gas that pervades the interstellar space. However, the details of how molecular clouds assemble from and interact with the atomic gas are still largely unknown. As a result of new observations of the 158 μm line of ionized carbon [CII] in the Cygnus region within the FEEDBACK program on SOFIA (Stratospheric Observatory for Infrared Astronomy), we present compelling evidence that [CII] unveils dynamic interactions between cloud ensembles. This process is neither a head-on collision of fully molecular clouds nor a gentle merging of only atomic clouds. Moreover, we demonstrate that the dense molecular clouds associated with the DR21 and W75N star-forming regions and a cloud at higher velocity are embedded in atomic gas, and all components interact over a large range of velocities (roughly 20 km s−1). The atomic gas has a density of around 100 cm−3 and a temperature of roughly 100 K. We conclude that the [CII] 158 μm line is an excellent tracer to witness the processes involved in cloud interactions and anticipate further detections of this phenomenon in other regions.

show abstract

The formation of young massive clusters by colliding flows

Cited by 41 publications

References 23 publications

The formation and early evolution of embedded star clusters in spiral galaxies

The formation and early evolution of embedded star clusters in spiral galaxies

The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds

Ionized carbon as a tracer of the assembly of interstellar clouds

Contact Info

Product

Resources

About