English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

It has been hypothesized that photons from young, massive star clusters areresponsible for maintaining the ionization of diffuse warm ionized gas seen inboth the Milky Way and other disk galaxies. For a theoretical investigation ofthe warm ionized medium (WIM), it is crucial to solve radiation transferequations where the ISM and clusters are modeled self-consistently. To thisend, we employ a Solar neighborhood model of TIGRESS, a magnetohydrodynamicsimulation of the multiphase, star-forming ISM, and post-process the simulationwith an adaptive ray tracing method to transfer UV radiation from starclusters. We find that the WIM volume filling factor is highly variable, andsensitive to the rate of ionizing photon production and ISM structure. The meanWIM volume filling factor rises to ~0.15 at |z|~1 kpc. Approximately half ofionizing photons are absorbed by gas and half by dust; the cumulative ionizingphoton escape fraction is 1.1%. Our time-averaged synthetic H$\alpha$ lineprofile matches WHAM observations on the redshifted (outflowing) side, but hasinsufficient intensity on the blueshifted side. Our simulation matches theDickey-Lockman neutral density profile well, but only a small fraction ofsnapshots have high-altitude WIM density consistent with Reynolds Layerestimates. We compute a clumping correction factor C = <n_e>/sqrt<n_e^2>~0.2that is remarkably constant with distance from the midplane and time; this canbe used to improve estimates of ionized gas mass and mean electron density fromobserved H$\alpha$ surface brightness profiles in edge-on galaxies.

Diffuse Ionized Gas in Simulations of Multiphase, Star-Forming Galactic Disks