Metallicity dependence of pressure-regulated feedback-modulated star formation in the tigress-ncr simulation suite

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dc.contributor.authorKim, Chang-Goo
dc.contributor.authorHassan, Sultan
dc.contributor.authorOstriker, Eve C
dc.date.accessioned2025-10-29T09:57:59Z
dc.date.available2025-10-29T09:57:59Z
dc.date.issued2024
dc.description.abstractWe present a new suite of numerical simulations of the star-forming interstellar medium (ISM) in galactic disks using the TIGRESS-NCR framework. Distinctive aspects of our simulation suite are: (1) sophisticated and comprehensive numerical treatments of essential physical processes including magnetohydrodynamics, self-gravity, and galactic differential rotation, as well as photochemistry, cooling, and heating coupled with direct ray-tracing UV radiation transfer and resolved supernova feedback and (2) wide parameter coverage including variation in metallicity over Z ′ ≡ Z/Z⊙ ∼ 0.1 − 3, gas surface density Σgas ∼ 5−150 M⊙ pc−2 , and stellar surface density Σstar ∼ 1−50 M⊙ pc−2 . The range of emergent star formation rate (SFR) surface density range is ΣSFR ∼ 10−4 − 0.5 M⊙ kpc−2 yr−1 and ISM total midplane pressure is Ptot/kB = 103 − 106 cm−3 K, with Ptot equal to the ISM weight W. For given Σgas and Σstar, we find ΣSFR ∝ Z ′0.3 . We provide an interpretation based on the pressureregulated feedback-modulated (PRFM) star formation theory. The total midplane pressure consists of thermal, turbulent, and magnetic stresses. We characterize feedback modulation in terms of the yield Υ, defined as the ratio of each stress to ΣSFR. The thermal feedback yield varies sensitively with both weight and metallicity as Υth ∝ W−0.46Z ′−0.53, while the combined turbulent and magnetic feedback yield shows weaker dependence Υturb+mag ∝ W−0.22Z ′−0.18. The reduction in ΣSFR at low metallicity is due mainly to enhanced thermal feedback yield, resulting from reduced attenuation of UV radiation. With the metallicity-dependent calibrations we provide, PRFM theory can be used for a new subgrid star formation prescription in cosmological simulations where the ISM is unresolved.
dc.identifier.citationKim, C.G., Ostriker, E.C., Kim, J.G., Gong, M., Bryan, G.L., Fielding, D.B., Hassan, S., Ho, M., Jeffreson, S.M., Somerville, R.S. and Steinwandel, U.P., 2024. Metallicity Dependence of Pressure-Regulated Feedback-Modulated Star Formation in the TIGRESS-NCR Simulation Suite. arXiv preprint arXiv:2405.19227.
dc.identifier.urihttps://doi.org/10.48550/arXiv.2405.19227
dc.identifier.urihttps://hdl.handle.net/10566/21221
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subjectInterstellar medium
dc.subjectStar formation
dc.subjectStellar feedback
dc.subjectMagnetohydrodynamical simulations
dc.subjectRadiative transfer simulations
dc.titleMetallicity dependence of pressure-regulated feedback-modulated star formation in the tigress-ncr simulation suite
dc.typeArticle

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