Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2009-05-25
Astrophys.J.699:L108-L112,2009
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
18pages, 4 figures, accepted for publication in Astrophysical Journal Letter
Scientific paper
10.1088/0004-637X/699/2/L108
We calculate the evolution of molecular line profiles of HCO$^+$ and C$^{18}$O toward a dense core thatis forming inside a magnetized turbulent molecular cloud. Features of the profiles can be affected more significantly by coupled velocity and abundance structures in the outer region than those in the inner dense part of the core. The velocity structure at large radii is dominated by a turbulent flow nearby and accretion shocks onto the core, which resulting in the variation between inward and outward motions during the evolution of the core. The chemical abundance structure is significantly affected by the depletion of molecules in the central region with high density and low temperature. During the evolution of the core, the asymmetry of line profiles easily changes from blue to red, and vice versa. According to our study, the observed reversed (red) asymmetry toward some starless cores could be interpreted as an intrinsic result of outward motion in the outer region of a dense core, which is embedded in a turbulent environment and still grows in density at the center.
Kim Jongsoo
Lee Jeong-Eun
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