Bursting Bubbles: Feedback from Clustered Supernovae and the Trade-off Between Turbulence and Outflows
Abstract
We present an analytic model for clustered supernovae (SNe) feedback in galaxy disks, incorporating the dynamical evolution of superbubbles formed from spatially overlapping SNe remnants. We propose two realistic outcomes for the evolution of superbubbles in galactic disks: (1) the expansion velocity of the shock front falls below the turbulent velocity dispersion of the interstellar medium in the galaxy disk, whereupon the superbubble stalls and fragments, depositing its momentum entirely within the galaxy disk; or (2) the superbubble grows in size to reach the gas scale height, breaking out of the galaxy disk and driving galactic outflows/fountains. In either case, we find that superbubble breakup/breakout almost always occurs before the last Type II SN (≲40 Myr) in the recently formed star cluster, assuming a standard high-end initial mass function slope, and scalings between stellar lifetimes and masses. The threshold between these two cases implies a break in the effective strength of feedback in driving turbulence within galaxies, and a resulting change in the scalings of, for example, star formation rates with gas surface density (the Kennicutt–Schmidt relation) and the star formation efficiency in galaxy disks.
Additional Information
© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 September 23; revised 2022 March 22; accepted 2022 May 1; published 2022 June 17. M.E.O. is grateful for the encouragement of his late father, S.R.O., in studying astrophysics. We thank Alex Gurvich, Lee Armus, and Phil Hopkins for conversations relating this model to disk formation at intermediate redshifts, and connections with spatially resolved observations and superwinds. We also would like to thank the anonymous reviewer for their comments that greatly improved the manuscript. M.E.O. was supported by the National Science Foundation Graduate Research Fellowship under grant No. 1144469. The Flatiron Institute is supported by the Simons Foundation. We thank Lucy Reading-Ikkanda/Simons Foundation for assistance with developing Figure 1. This research has made use of NASA's Astrophysics Data System. B.B. is grateful for support from the Packard Fellowship and Sloan Fellowship.Attached Files
Published - Orr_2022_ApJ_932_88.pdf
Accepted Version - 2109.14656.pdf
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Additional details
- Eprint ID
- 115771
- Resolver ID
- CaltechAUTHORS:20220722-768845000
- DGE-1144469
- NSF Graduate Research Fellowship
- Simons Foundation
- David and Lucile Packard Foundation
- Alfred P. Sloan Foundation
- Created
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2022-07-26Created from EPrint's datestamp field
- Updated
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2022-07-26Created from EPrint's last_modified field
- Caltech groups
- TAPIR