Star formation on the move?
Walsh, Andrew J., Myers, Philip C., and Burton, Michael G. (2004) Star formation on the move? Astrophysical Journal: an international review of astronomy and astronomical physics, 614 (1). pp. 194-202.
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View at Publisher Website: http://dx.doi.org/10.1086/423425
Recent models of star formation suggest that the mass of a star is largely determined by its history of motion through its natal molecular cloud. Such motions may be observable in the early stages of star formation. We have looked for the relative shifts of line-center velocity in low [13CO (1-0) and C18O (1-0)] and high [N2H+ (1-0)] density tracers toward a sample of 42 low-mass star-forming cores. Our results indicate that any motions of the high-density cores with respect to their low-density envelopes are very small (<~0.1 km s-1) compared to the motions expected from models of ballistic movement. We therefore conclude that isolated cores do not generally move ballistically with respect to their surrounding envelopes.
|Item Type:||Article (Refereed Research - C1)|
|Keywords:||ISM: clouds; kinematics and dynamics; stars: formation|
|FoR Codes:||02 PHYSICAL SCIENCES > 0201 Astronomical and Space Sciences > 020104 Galactic Astronomy @ 100%|
|SEO Codes:||97 EXPANDING KNOWLEDGE > 970102 Expanding Knowledge in the Physical Sciences @ 100%|
|Deposited On:||16 Mar 2010 09:42|
|Last Modified:||18 Oct 2013 00:57|
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