Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way

Kolborg, A. N.; Martizzi, Davidé; Ramírez-Ruiz, E.; Pfister, Hugo; Sakari, Charli M.; Soares-Furtado, Melinda

doi:10.3847/2041-8213/ac8c98

Cited by 4 publications

(15 citation statements)

References 48 publications

(83 reference statements)

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“…We use the hydrodynamic code RAMSES (Teyssier 2002) to simulate the evolution of gas in patches of galactic disks over timescales of hundreds of millions of years. The fundamental simulation setup is the same as that used in Martizzi et al (2016) and Kolborg et al (2022), with the inclusion of a passive scalar field in order to trace the enrichment of r-process elements. In this section, we describe the salient aspects of the models as they pertain to this project.…”

Section: Methodsmentioning

confidence: 99%

“…In this section, we describe the salient aspects of the models as they pertain to this project. For additional details, we refer the interested reader to Martizzi et al (2016) and Kolborg et al (2022). The full suite of simulations used in this study are listed in Table 1.…”

Section: Methodsmentioning

confidence: 99%

“…The simulations assume a static gravitational potential produced by gas, stars, and dark matter as described by Kuijken & Gilmore (1989). The parameters of this gravitational potential are varied to emulate three different types of galaxies (Kolborg et al 2022).…”

Section: Galaxy Modelsmentioning

confidence: 99%

“…A central goal of this paper is to use a series of idealized hydrodynamic simulations of the response of galactic disks to SN feedback and metal mixing (Kolborg et al 2022) to provide a deeper physical interpretation of the star-to-star r-process scatter observed in the MW in the metallicity extent [Fe/H] of approximately −3.0 to −1.5, where Fe enrichment is driven primarily by cc-SNe (Hotokezaka et al 2018;Côté et al 2019;Wanajo et al 2021). The constraints derived from the abundance pattern of r-process elements in the MW may ultimately help decipher the dominant production mechanism in the early universe.…”

Section: Introductionmentioning

confidence: 99%

“…In preference, in this paper we propose to model the gas interactions in small patches of galaxy disk simulations in order to effectively isolate the small-scale mixing effects of metals at subparsec scales from cc-SNe and rprocess-producing events (such as neutron star mergers, NSMs) into the interstellar medium (ISM). Besides being computationally workable (Kolborg et al 2022), investigating the distribution of r-process elements in these simulations and comparing them extensively with observational data of metalpoor stars can, in turn, help constrain the frequency of events and the mass content of r-process material per event.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on the Frequency and Mass Content of r-process Events Derived from Turbulent Mixing in Galactic Disks

Kolborg

Ramírez-Ruiz

Martizzi

et al. 2023

ApJ

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Metal-poor stars in the Milky Way (MW) halo display large star-to-star dispersion in their r-process abundance relative to lighter elements. This suggests a chemically diverse and unmixed interstellar medium (ISM) in the early universe. This study aims to help shed light on the impact of turbulent mixing, driven by core-collapse supernovae (cc-SNe), on the r-process abundance dispersal in galactic disks. To this end, we conduct a series of simulations of small-scale galaxy patches which resolve metal-mixing mechanisms at parsec scales. Our setup includes cc-SNe feedback and enrichment from r-process sources. We find that the relative rate of the r-process events to cc-SNe is directly imprinted on the shape of the r-process distribution in the ISM with more frequent events causing more centrally peaked distributions. We consider also the fraction of metals that is lost on galactic winds and find that cc-SNe are able to efficiently launch highly enriched winds, especially in smaller galaxy models. This result suggests that smaller systems, e.g., dwarf galaxies, may require higher levels of enrichment in order to achieve similar mean r-process abundances as MW-like progenitors systems. Finally, we are able to place novel constraints on the production rate of r-process elements in the MW, 6 × 10 − 7 M ⊙ yr − 1 ≲ m ̇ rp ≪ 4.7 × 10 − 4 M ⊙ yr − 1 , imposed by accurately reproducing the mean and dispersion of [Eu/Fe] in metal-poor stars. Our results are consistent with independent estimates from alternate methods and constitute a significant reduction in the permitted parameter space.

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Galaxy Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Constraints on the Frequency and Mass Content of r-process Events Derived from Turbulent Mixing in Galactic Disks

Kolborg

Ramírez-Ruiz

Martizzi

et al. 2023

ApJ

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The ratio of [Eu/α] differentiates accreted/in situ Milky Way stars across metallicities, as indicated by both field stars and globular clusters

Monty,

Belokurov,

Sanders

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We combine stellar orbits with the abundances of the heavy, r-process element europium and the light, α-element, silicon to separate in-situ and accreted populations in the Milky Way across all metallicities. At high orbital energy, the accretion-dominated halo shows elevated values of [Eu/Si], while at lower energies, where many of the stars were born in-situ, the levels of [Eu/Si] are lower. These systematically different levels of [Eu/Si] in the MW and the accreted halo imply that the scatter in [Eu/α] within a single galaxy is smaller than previously thought. At the lowest metallicities, we find that both accreted and in-situ populations trend down in [Eu/Si], consistent with enrichment via neutron star mergers. Through compiling a large dataset of abundances for 54 globular clusters (GCs), we show that differences in [Eu/Si] extend to populations of in-situ/accreted GCs. We interpret this consistency as evidence that in r-process elements GCs trace the star formation history of their hosts, motivating their use as sub-Gyr timers of galactic evolution. Furthermore, fitting the trends in [Eu/Si] using a simple galactic chemical evolution model, we find that differences in [Eu/Si] between accreted and in-situ MW field stars cannot be explained through star formation efficiency alone. Finally, we show that the use of [Eu/Si] as a chemical tag between GCs and their host galaxies extends beyond the Local Group, to the halo of M31 - potentially offering the opportunity to do Galactic Archaeology in an external galaxy.

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Spectacular Nucleosynthesis from Early Massive Stars

Ji,

Curtis,

Storm

et al. 2024

ApJL

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Stars that formed with an initial mass of over 50 M ⊙ are very rare today, but they are thought to be more common in the early Universe. The fates of those early, metal-poor, massive stars are highly uncertain. Most are expected to directly collapse to black holes, while some may explode as a result of rotationally powered engines or the pair-creation instability. We present the chemical abundances of J0931+0038, a nearby low-mass star identified in early follow-up of the SDSS-V Milky Way Mapper, which preserves the signature of unusual nucleosynthesis from a massive star in the early Universe. J0931+0038 has a relatively high metallicity ([Fe/H] = −1.76 ± 0.13) but an extreme odd–even abundance pattern, with some of the lowest known abundance ratios of [N/Fe], [Na/Fe], [K/Fe], [Sc/Fe], and [Ba/Fe]. The implication is that a majority of its metals originated in a single extremely metal-poor nucleosynthetic source. An extensive search through nucleosynthesis predictions finds a clear preference for progenitors with initial mass >50 M ⊙, making J0931+0038 one of the first observational constraints on nucleosynthesis in this mass range. However, the full abundance pattern is not matched by any models in the literature. J0931+0038 thus presents a challenge for the next generation of nucleosynthesis models and motivates the study of high-mass progenitor stars impacted by convection, rotation, jets, and/or binary companions. Though rare, more examples of unusual early nucleosynthesis in metal-poor stars should be found in upcoming large spectroscopic surveys.

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Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way

Cited by 4 publications

References 48 publications

Constraints on the Frequency and Mass Content of r-process Events Derived from Turbulent Mixing in Galactic Disks

Constraints on the Frequency and Mass Content of r-process Events Derived from Turbulent Mixing in Galactic Disks

The ratio of [Eu/α] differentiates accreted/in situ Milky Way stars across metallicities, as indicated by both field stars and globular clusters

Spectacular Nucleosynthesis from Early Massive Stars

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