Radiation-pressure-driven dust transport to galaxy halos at $zsim 10$. (arXiv:1905.05645v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hirashita_H/0/1/0/all/0/1">Hiroyuki Hirashita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inoue_A/0/1/0/all/0/1">Akio K. Inoue</a>
The origin of dust in galaxy halos or in the circum-galactic medium (CGM) is
still a mystery. We investigate if the radiation pressure in high-redshift
($zsim 10$) galaxies can efficiently transport dust to halos. To clarify the
first dust enrichment of galaxy halos in the early Universe, we solve the
motion of a dust grain considering radiation pressure, gas drag, and gravity in
the vertical direction of the galactic disc. Radiation pressure is estimated in
a consistent manner with the stellar spectra and dust extinction. As a
consequence, we find that dust grains with radii $asim 0.1~mu$m successfully
escape from the galactic disc if the ongoing star formation episode converts
more than 15 per cent of the baryon content into stars and lasts $gtrsim 30$
Myr, while larger and smaller grains are trapped in the disc because of gravity
and gas drag, respectively. We also show that grain charge significantly
enhances gas drag at a few–10 scale heights of the galactic disc, where the
grain velocities are suppressed to $sim 1$ km s$^{-1}$. There is an optimum
dust-to-gas ratio ($sim 10^{-3}$) in the galactic disc and an optimum virial
mass $sim 10^{10}$–$10^{11}$ M$_{odot}$ for the transport of $asim
0.1~mu$m grains to the halo. We conclude that early dust enrichment of galaxy
halos at $zgtrsim 10$ is important for the origin of dust in the CGM.
The origin of dust in galaxy halos or in the circum-galactic medium (CGM) is
still a mystery. We investigate if the radiation pressure in high-redshift
($zsim 10$) galaxies can efficiently transport dust to halos. To clarify the
first dust enrichment of galaxy halos in the early Universe, we solve the
motion of a dust grain considering radiation pressure, gas drag, and gravity in
the vertical direction of the galactic disc. Radiation pressure is estimated in
a consistent manner with the stellar spectra and dust extinction. As a
consequence, we find that dust grains with radii $asim 0.1~mu$m successfully
escape from the galactic disc if the ongoing star formation episode converts
more than 15 per cent of the baryon content into stars and lasts $gtrsim 30$
Myr, while larger and smaller grains are trapped in the disc because of gravity
and gas drag, respectively. We also show that grain charge significantly
enhances gas drag at a few–10 scale heights of the galactic disc, where the
grain velocities are suppressed to $sim 1$ km s$^{-1}$. There is an optimum
dust-to-gas ratio ($sim 10^{-3}$) in the galactic disc and an optimum virial
mass $sim 10^{10}$–$10^{11}$ M$_{odot}$ for the transport of $asim
0.1~mu$m grains to the halo. We conclude that early dust enrichment of galaxy
halos at $zgtrsim 10$ is important for the origin of dust in the CGM.
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