The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert

Grudić, Michael Y.; Guszejnov, Dávid; Offner, Stella S. R.; Rosen, Anna L.; Raju, Aman N.; Faucher-Giguère, Claude-André; Hopkins, Philip F.

doi:10.48550/arxiv.2201.00882

Cited by 8 publications

(16 citation statements)

References 131 publications

(201 reference statements)

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“…Finally, we conclude that both gravity and outflow feedback affect the velocity field, driving larger velocity dispersion in star-forming regions. In particular, outflows enhance fragmentation (Federrath et al 2014b;Mathew & Federrath 2021;Grudić et al 2022). Compared with gravity, the outflow has its effect on larger scales up to ∼ 1 pc at least (see Fig.…”

Section: The Structure Function Of Dense Star-forming Regionsmentioning

confidence: 98%

The Velocity Statistics of Turbulent Clouds in the Presence of Gravity, Magnetic fields, Radiation, and Outflow Feedback

Hu,

Federrath,

et al. 2022

Preprint

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The interaction of turbulence, magnetic fields, self-gravity, and stellar feedback within molecular clouds is crucial for understanding star formation. We study the effects of self-gravity and outflow feedback on the properties of the turbulent velocity via the structure function over length scales from ∼ 0.01 pc to 2 pc. We analyse a series of three-dimensional, magnetohydrodynamical (MHD) simulations of star cluster formation, including self-gravity, turbulence, magnetic fields, stellar radiative heating, and outflow feedback. We observe that self-gravity and protostellar outflows increase the velocity fluctuations over all length scales. In particular, outflows can amplify the velocity fluctuations by up to a factor of 7 on scales ∼ 0.01 -0.2 pc and drive turbulence up to a scale of ∼ 1 pc. The amplified velocity fluctuations provide more support against gravity and enhance fragmentation on small scales. The role of self-gravity is more significant on smaller dense clumps and it increases the fraction of the compressive velocity component up to a scale of ∼ 0.2 pc. However, outflow feedback drives both solenoidal and compressive modes, but it induces a higher fraction of solenoidal modes relative to compressive modes. Thus, with outflows, the dense core ends up with a slightly higher fraction of solenoidal modes. We find that the compressible fraction is fairly constant with about 1/3 on scales ∼ 0.1 -0.2 pc. The combined effect of enhanced velocity dispersion and reduced compressive fraction contributes to a reduction in the star formation rate compared to when outflow feedback is not included.

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Section: The Structure Function Of Dense Star-forming Regionsmentioning

confidence: 98%

The Velocity Statistics of Turbulent Clouds in the Presence of Gravity, Magnetic fields, Radiation, and Outflow Feedback

Hu,

Federrath,

et al. 2022

Preprint

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“…With all the approaches to SN feedback, the majority of lowmass clusters have finished their accretion before the onset of SNe at 3-4 Myr, leading to little difference in the durations between our approaches. Such short durations indicate that the other sources of feedback are able to terminate cluster formation before the start of SN feedback (Kruĳssen et al 2019;Grudić et al 2022). SN feedback remains more relevant for massive clusters.…”

Section: Timing Of Supernova Feedbackmentioning

confidence: 99%

“…However, this assumption may be incorrect. For example, using a simulation of a star cluster forming out of a 2×10 4 M GMC, Grudić et al (2022) find that massive stars (𝑚 > 10 M ) finish accreting 1 Myr later than the average star. Padoan et al (2020) of SN, they do not account for this systematic delay in the formation of individual stars.…”

Section: Timing Of Supernova Feedbackmentioning

confidence: 99%

“…However, it may need to be further refined to account for the delay in massive star formation. In particular, one possible approach would be to calibrate a subgrid model for the timing of cluster feedback to the results of GMC-scale simulations such as in Grudić et al (2022). Further delays in the onset of massive star feedback may increase the timescales of cluster formation and the integrated star formation efficiency, but these effects are likely to be small compared to the effects of other parameters, namely 𝜖 ff .…”

Section: Timing Of Supernova Feedbackmentioning

confidence: 99%

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Testing Feedback from Star Clusters in Simulations of the Milky Way Formation

Brown,

Gnedin

2022

Preprint

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We present a suite of galaxy formation simulations that directly model star cluster formation and disruption. Starting from a model previously developed by our group, here we introduce several improvements to the prescriptions for cluster formation and feedback, then test these updates using a large suite of cosmological simulations of Milky Way mass galaxies. We perform a differential analysis with the goal of understanding how each of the updates affects star cluster populations. Two key parameters are the momentum boost of supernova feedback 𝑓 boost and star formation efficiency per freefall time 𝜖 ff . We find that 𝑓 boost has a strong influence on the galactic star formation rate, with higher values leading to less star formation. The efficiency 𝜖 ff does not have a significant impact on the global star formation rate, but dramatically changes cluster properties, with increasing 𝜖 ff leading to a higher maximum cluster mass, shorter age spread of stars within clusters, and higher integrated star formation efficiencies. We also explore the redshift evolution of the observable cluster mass function, finding that most massive clusters have formed at high redshift 𝑧 > 4. Extrapolation of cluster disruption to 𝑧 = 0 produces good agreement with both the Galactic globular cluster mass function and age-metallicity relation. Our results emphasize the importance of using small-scale properties of galaxies to calibrate subgrid models of star cluster formation and feedback.

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“…Clarke & Pringle 1993;Pfalzner et al 2005;Rosotti et al 2014; Dai ★ E-mail: lin.qiao@qmul.ac.uk 1 https://exoplanetarchive.ipac.caltech.edu/ et al 2015; Vincke & Pfalzner 2016;Rodriguez et al 2018;Winter et al 2018a;Cuello et al 2019Cuello et al , 2020Parker 2020). In massive stellar clusters, massive stars also form, which emit large amounts of UV photons that photoionise and disperse the star forming cloud (McKee 1989;Walch et al 2012;Dale et al 2014;Geen et al 2015Geen et al , 2016Ali et al 2018;Ali 2021;Grudić et al 2021Grudić et al , 2022. This injection of energy into the surroundings is called "feedback" and the main focus of prior simulations into this has been the effect on the star formation within clouds.…”

Section: Introductionmentioning

confidence: 99%

The evolution of protoplanetary discs in star formation and feedback simulations

Qiao,

Haworth,

Sellek

et al. 2022

Preprint

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We couple star cluster formation and feedback simulations of a Carina-like star forming region with 1D disc evolutionary models to study the impact of external photoevaporation on disc populations in massive star forming regions. To investigate the effect of shielding of young stellar objects by star forming material, we track the FUV field history at each star in the cluster with two methods: i) Monte Carlo radiative transfer accounting for the shielding of stars from the FUV by the star forming cloud ii) Geometric dilution of the radiation from other stars which ignores shielding effects. We found that significant shielding only occurs for a small fraction of discs and offers protection from external photoevaporation for < 0.5 Myr. However, this initial protection can prevent significant early gas/dust mass loss and disc radius reduction due to external photoevaporation. Particularly, shielding for 0.5 Myr is sufficient for much of the solid reservoir to evolve to larger sizes where it will not be entrained in an external wind. Shielding is therefore potentially significant for terrestrial planet formation in retaining the solid mass budget, but the continued stripping of gas when shielding ends could still impact migration and the gas reservoir for giant planet atmospheres. Our models highlight issues with treating all discs in a cluster with a single characteristic age, since shielded objects are typically only the youngest. Our model predicts that the majority of discs in a 2 Myr Carina-like environment are subject to strong external photoevaporation.

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The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert

Cited by 8 publications

References 131 publications

The Velocity Statistics of Turbulent Clouds in the Presence of Gravity, Magnetic fields, Radiation, and Outflow Feedback

The Velocity Statistics of Turbulent Clouds in the Presence of Gravity, Magnetic fields, Radiation, and Outflow Feedback

Testing Feedback from Star Clusters in Simulations of the Milky Way Formation

The evolution of protoplanetary discs in star formation and feedback simulations

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