Turbulent Properties in Star-forming Molecular Clouds Down to the Sonic Scale. II. Investigating the Relation between Turbulence and Star-forming Environments in Molecular Clouds
Abstract We investigate the effect of star formation on turbulence in the Orion A and Ophiuchus clouds using principal component analysis (PCA). We measure the properties of turbulence by applying PCA on the spectral maps in 13 CO, C 18 O, HCO + J = 1–0, and CS J = 2–1. First, the scaling relations...
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Published in | The Astrophysical journal Vol. 921; no. 1; pp. 31 - 45 |
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Main Authors | , , , , , , , , , , , , , , , , |
Format | Journal Article |
Language | English |
Published |
Philadelphia
The American Astronomical Society
01.11.2021
IOP Publishing |
Subjects | |
Online Access | Get full text |
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Summary: | Abstract
We investigate the effect of star formation on turbulence in the Orion A and Ophiuchus clouds using principal component analysis (PCA). We measure the properties of turbulence by applying PCA on the spectral maps in
13
CO, C
18
O, HCO
+
J
= 1–0, and CS
J
= 2–1. First, the scaling relations derived from PCA of the
13
CO maps show that the velocity difference (
δv
) for a given spatial scale (
L
) is the highest in the integral-shaped filament (ISF) and L1688, where the most active star formation occurs in the two clouds. The
δv
increases with the number density and total bolometric luminosity of the protostars in the subregions. Second, in the ISF and L1688 regions, the
δv
of C
18
O, HCO
+
, and CS are generally higher than that of
13
CO, which implies that the dense gas is more turbulent than the diffuse gas in the star-forming regions; stars form in dense gas, and dynamical activities associated with star formation, such as jets and outflows, can provide energy into the surrounding gas to enhance turbulent motions. |
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Bibliography: | AAS31428 Interstellar Matter and the Local Universe |
ISSN: | 0004-637X 1538-4357 |
DOI: | 10.3847/1538-4357/ac193e |