Extended Hot Gas Halos Around Starburst Galaxies
Kohji Tomisaka, Joel N. Bregman

TL;DR
This paper models the extended X-ray emission around starburst galaxy M82 using hydrodynamic simulations, explaining the evolution of wind-driven bubbles and shock fronts over time and their observable X-ray luminosities.
Contribution
It provides a detailed hydrodynamic simulation of starburst-driven outflows extending into the halo, linking physical processes to observed X-ray emissions.
Findings
Outflows reach 40-50 kpc in 50 Myr for halo density of 10^{-3} cm^{-3}
X-ray luminosity ranges from 3×10^{39} to 10^{41} erg/s depending on the band
Three evolutionary stages of wind-blown bubbles are identified
Abstract
Reanalysis of Einstein IPC data and new observations from the GINGA LAC indicate the presence of extended X-ray emission (10-50 kpc) around the starburst galaxy M82. Here we model this emission by calculating numerical hydrodynamic simulations of the starburst event to much later times and larger scales than previously considered. For our models, we adopt a supernova rate of 0.1 , and an extended low-density static halo that is bound to the galaxy. There are three stages to the evolution of the wind-blown bubble and the propagation of the shock front: the bubble expands in an almost uniform density disk gas, with a deceleration of the shock front ( 3.6 Myr); breakout from the disk and the upward acceleration of the shock front (3.6 Myr 18 Myr); propagation into the halo, leading to a more spherical system and shock deceleration (18 Myr $\alt…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
Taxonomy
TopicsAstrophysics and Star Formation Studies · Astronomy and Astrophysical Research · Stellar, planetary, and galactic studies
