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Radiatively Cooling Superwinds in Ultracompact Hii Regions

Published online by Cambridge University Press:  09 June 2023

A. Danehkar Open the ORCID record for A. Danehkar [Opens in a new window]
A. Danehkar*
Affiliation:
Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USA email:danehkar@eurekasci.com
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Abstract

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Ultracompact Hii regions (UC-HII) are the young, very dense cores of massive star-forming regions in dwarf galaxies, where newly formed massive OB stars are surrounded by natal molecular clouds. Thermal energy deposited by mechanical feedback from a cluster of massive OB stars can form a superwind, which may lead to a wind-blown bubble as well as radiative cooling. We investigate the formation of radiatively cooling superwinds in UC-HII using a radiative cooling module in the hydrodynamics program. We built a grid of hydrodynamic simulations to determine the dependence of radiative cooling on the cluster radius, mass-deposition rate, wind velocity, and ambient medium in UC-HII. Our findings could help to better understand star formation in massive star-forming regions, where cool superwinds could trigger the formation of molecular clumpy regions.

Keywords

Stars: windsISM: bubblesradiation mechanismsgalaxies: starburst
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 25 - 27
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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