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research
Turbulence in giant molecular clouds: the effect of photoionization feedback
Authors
B. Ercolano
Ballesteros-Paredes
+74 more
Ballesteros-Paredes
Ballesteros-Paredes
Bate
Brunt
Cunningham
D. M. Boneberg
Dale
Dale
Dale
Dale
Dale
Dobbs
Dobbs
Dobbs
Dobbs
Elmegreen
Falgarone
Federrath
Federrath
Federrath
Federrath
Federrath
Federrath
Federrath
Federrath
Federrath
Girichidis
Girichidis
Goldbaum
Gritschneder
Heitsch
Hennebelle
Hennebelle
Hennebelle
Heyer
J. E. Dale
Kainulainen
Kainulainen
Kainulainen
Klessen
Klessen
Kolmogorov
Konstandin
Kritsuk
Krumholz
Krumholz
Krumholz
Krumholz
Li
Mac Low
Mac Low
McKee
Molina
Myers
Offner
Ossenkopf
P. Girichidis
Padoan
Padoan
Passot
Price
Rogers
Roman-Duval
Schmidt
Schneider
Schneider
Tasker
Vazquez-Semadeni
Vázquez-Semadeni
Vázquez-Semadeni
Vázquez-Semadeni
Walch
Wang
Zuckerman
Publication date
21 February 2015
Publisher
'Oxford University Press (OUP)'
Doi
Cite
Abstract
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.Giant molecular clouds (GMCs) are observed to be turbulent, but theory shows that without a driving mechanism turbulence should quickly decay. The question arises by which mechanisms turbulence is driven or sustained. It has been shown that photoionizing feedback from massive stars has an impact on the surrounding GMC and can for example create vast H II bubbles. We therefore address the question of whether turbulence is a consequence of this effect of feedback on the cloud. To investigate this, we analyse the velocity field of simulations of high-mass star-forming regions by studying velocity structure functions and power spectra. We find that clouds whose morphology is strongly affected by photoionizing feedback also show evidence of driving of turbulence by preserving or recovering a Kolmogorov-type velocity field. On the contrary, control run simulations without photoionizing feedback have a velocity distribution that bears the signature of gravitational collapse and of the dissipation of energy, where the initial Kolmogorov-type structure function is erased.Peer reviewe
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info:doi/10.1093%2Fmnras%2Fstu...
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