Rowan J Smith


Revealing the dynamics of star formation in filaments and in massive star-forming regions.

Rahul Shetty, Amy Stutz


While classical theoretical models of star-forming regions were spherical, recent Herschel observations have shown that star forming cores are typically both asymmetric, and embedded within filaments. Accordingly, radiative transfer models of such regions must be increased in complexity to find meaningful diagnostics of where gravitational collapse is underway.

In this contribution, I will use radiative transfer modeling of filaments and massive star-forming regions within a clustered molecular cloud simulation, to reveal the line profiles of collapsing clumps and cores. I will show in which tracers a double peaked line profile with a blue asymmetry remains a robust tracer of collapse for low mass filamentary cores. I find that massive star-forming regions have a unique line-of-sight velocity profile. The resulting line profiles this produces are very early indicators of massive star formation, and provide critical observational diagnostics of how massive stars are assembled.