8-12 juin, 2014


Filaments and Star Formation

Helen Kirk (NRC-Herzberg)

Mikhail Klassen (McMaster University) Samantha Pillsworth (St Mary's University Ralph Pudritz (McMaster University)

Observations from the Herschel Space Telescope have highlighted the prevalence and importance of filaments in the star formation process. Most young forming stars appear to be associated with filaments, and young stellar clusters often lie at the intersection point of several filaments. Much remains to be learned about the filaments themselves - for example, are they stable, quasi-equilibrium objects, or do they rapidly evolve? We first turn to numerical simulations of star formation which form filaments that appear similar to observed filaments. Using the simulations, we gain insight into the competing effects of magnetic fields, turbulence, and gravity on the formation and evolution of the filaments. Even the weak magnetic fields adopted in the simulation are enough to play a strong role in shaping the emergent filaments, leading to puffier, wider filaments than in the non-magnetic case. Furthermore, we find that not all of the filaments formed are stable, long-lived entities; some filaments are found to form and disperse in just a few tenths of a Myr. We compare some of the features of the simulated filaments with those found in the nearby Orion molecular cloud observed as part of the JCMT Gould Belt Survey.

Mode de présentation: 2014-06-09 13:45 (doit être confirmé par le SOC)