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Radiative Stellar Feedback in Galaxy Formation: Methods and Physics

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arxiv 1811.12462 v2 pith:AZJFYRFQ submitted 2018-11-29 astro-ph.GA astro-ph.COastro-ph.IM

Philip F. Hopkins (Caltech) , Michael Y. Grudic (Caltech) , Andrew R. Wetzel (UC Davis) , Dusan Keres (UCSD) , Claude-Andre Gaucher-Giguere (Northwestern) , Xiangcheng Ma (UC Berkeley) , Norman Murray (CITA) , Nathan Butcher (UCSD) This is my paper · ORCID
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keywords galaxiesphoto-ionizationfeedbackformationheatingstarwhendwarfs
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Radiative feedback (RFB) from stars plays a key role in galaxies, but remains poorly-understood. We explore this using high-resolution, multi-frequency radiation-hydrodynamics (RHD) simulations from the Feedback In Realistic Environments (FIRE) project. We study ultra-faint dwarf through Milky Way mass scales, including H+He photo-ionization; photo-electric, Lyman Werner, Compton, and dust heating; and single+multiple scattering radiation pressure (RP). We compare distinct numerical algorithms: ray-based LEBRON (exact when optically-thin) and moments-based M1 (exact when optically-thick). The most important RFB channels on galaxy scales are photo-ionization heating and single-scattering RP: in all galaxies, most ionizing/far-UV luminosity (~1/2 of lifetime-integrated bolometric) is absorbed. In dwarfs, the most important effect is photo-ionization heating from the UV background suppressing accretion. In MW-mass galaxies, meta-galactic backgrounds have negligible effects; but local photo-ionization and single-scattering RP contribute to regulating the galactic star formation efficiency and lowering central densities. Without some RFB (or other 'rapid' FB), resolved GMCs convert too-efficiently into stars, making galaxies dominated by hyper-dense, bound star clusters. This makes star formation more violent and 'bursty' when SNe explode in these hyper-clustered objects: thus, including RFB 'smoothes' SFHs. These conclusions are robust to RHD methods, but M1 produces somewhat stronger effects. Like in previous FIRE simulations, IR multiple-scattering is rare (negligible in dwarfs, ~10% of RP in massive galaxies): absorption occurs primarily in 'normal' GMCs with A_v~1.

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Cited by 2 Pith papers

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    Local photoionization feedback from a galaxy's own stars and hot gas reduces final stellar mass by about 20 percent and HI mass by about 50 percent in simulated galaxies spanning dwarf to massive spiral masses.

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