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Infrared appearance of wind-blown bubbles around young massive stars

Published online by Cambridge University Press:  20 January 2023

Maria S. Kirsanova Open the ORCID record for Maria S. Kirsanova [Opens in a new window]  and
Yaroslav N. Pavlyuchenkov
Maria S. Kirsanova
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, 119017, 48 Pyatnitskaya str., Moscow, Russia email: [email protected]
Yaroslav N. Pavlyuchenkov
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, 119017, 48 Pyatnitskaya str., Moscow, Russia email: [email protected]
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Abstract

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Thousands of ring-like bubbles appear on infrared images of the Galaxy plane. Most of these infrared bubbles form during expansion of Hii regions around massive stars. However, the physical effects that determine their morphology are still under debate. Namely, the absence of the infrared emission toward the centres of the bubbles can be explained by pushing the dust grains by stellar radiation pressure. At the same time, small graphite grains and PAHs are not strongly affected by the radiation pressure and must be removed by another process. Stellar ultraviolet emission can destroy the smallest PAHs but the photodestruction is ineffective for the large PAHs. Meanwhile, the stellar wind can evacuate all types of grains from Hii regions. In the frame of our chemo-dynamical model we vary parameters of the stellar wind and illustrate their influence on the morphology and synthetic infrared images of the bubbles.

Keywords

ISM: bubblesISM: dustextinctionISM: HII regionsstars: windsoutflows
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 268 - 272
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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