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The Accretion of Fuel at the Disk-Halo Interface

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arxiv 0907.1023 v1 pith:PV53RZ24 submitted 2009-07-06 astro-ph.GA astro-ph.CO

M.E. Putman , J.E.G. Peek , F. Heitsch This is my paper · ORCID
classification astro-ph.GAastro-ph.CO
keywords cloudscolddisk-halointerfacefuelgalaxyrecoolingaccretion
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We discuss the support for the cooling of gas directly at the disk-halo interface as a mechanism to continually fuel a galaxy. This may be an important reservoir as there is not enough cold gas observed in galaxy halos and simulations indicate the existing cold clouds will be rapidly destroyed as they move through the surrounding halo medium. We show possible evidence for a net infall of the WIM layer in the Milky Way, simulation results showing the recooling of warm clouds at the disk-halo interface, and GALFA HI data of small, cold HI clouds that could represent this recooling.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. The Warm-Hot Disk-Halo Interface Below the Perseus Spiral Arm

    astro-ph.GA 2025-02 conditional novelty 7.0 of 10

    First direct vertical profile of gas below the Perseus arm shows warm gas declining steeply with height while high-ion gas (Si IV, C IV) remains roughly constant, with a uniform C IV/Si IV ratio of 2.5.

  2. Milky Way Atlas: A radial-velocity-resolved, three-dimensional map of H I within 1.25 kpc

    astro-ph.GA 2026-07 unverdicted novelty 6.0 of 10

    A Bayesian inference method combining HI4PI radio data with Gaia-based 3D dust maps reconstructs the 3D density, velocity, and line-width of local atomic hydrogen within 1.25 kpc, validated by synthetic tests and inde...

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