%0 Generic %1 klassen2016filamentary %A Klassen, Mikhail %A Pudritz, Ralph E. %A Kirk, Helen %D 2016 %K DisPerSE Filaments Molecular %T Filamentary flow and magnetic geometry in evolving cluster-forming molecular cloud clumps %U http://arxiv.org/abs/1605.08835 %X We present an analysis of the relationship between the orientation of magnetic fields and filaments that form in 3D magnetohydrodynamic simulations of cluster-forming, turbulent molecular cloud clumps. We examine simulated cloud clumps with size scales of L ~ 2-4 pc and densities of n ~ 400-1000 cm^-3. Many molecular clouds have Alfven Mach numbers near unity, a regime insufficiently explored by numerical simulations. We simulated two cloud clumps of different masses, one in virial equilibrium, the other strongly gravitationally bound, but with the same initial turbulent velocity field and similar mass-to-flux ratio. We apply various techniques to analyze the filamentary and magnetic structure of the resulting cloud, including the DisPerSE filament-finding algorithm in 3D. The largest structure that forms is a 1-2 parsec-long filament, with smaller connecting sub-filaments. We find that in our trans-Alfvenic clouds, wherein magnetic forces and turbulence are comparable, coherent orientation of the magnetic field depends on the virial parameter. Subvirial clumps undergo strong gravitational collapse and magnetic field lines are dragged with the accretion flow. We see evidence of filament-aligned flow and accretion flow onto the filament in the subvirial cloud. Magnetic fields aligned more parallel in the subvirial cloud and more perpendicular in the denser, marginally bound cloud. Radiative feedback from a 16 Msun star forming in a cluster in one of our simulations results in the destruction of the main filament, the formation of an HII region, and the sweeping up of magnetic fields within an expanding shell of material at the edges of the HII region.

@misc{klassen2016filamentary, abstract = {We present an analysis of the relationship between the orientation of magnetic fields and filaments that form in 3D magnetohydrodynamic simulations of cluster-forming, turbulent molecular cloud clumps. We examine simulated cloud clumps with size scales of L ~ 2-4 pc and densities of n ~ 400-1000 cm^-3. Many molecular clouds have Alfven Mach numbers near unity, a regime insufficiently explored by numerical simulations. We simulated two cloud clumps of different masses, one in virial equilibrium, the other strongly gravitationally bound, but with the same initial turbulent velocity field and similar mass-to-flux ratio. We apply various techniques to analyze the filamentary and magnetic structure of the resulting cloud, including the DisPerSE filament-finding algorithm in 3D. The largest structure that forms is a 1-2 parsec-long filament, with smaller connecting sub-filaments. We find that in our trans-Alfvenic clouds, wherein magnetic forces and turbulence are comparable, coherent orientation of the magnetic field depends on the virial parameter. Subvirial clumps undergo strong gravitational collapse and magnetic field lines are dragged with the accretion flow. We see evidence of filament-aligned flow and accretion flow onto the filament in the subvirial cloud. Magnetic fields aligned more parallel in the subvirial cloud and more perpendicular in the denser, marginally bound cloud. Radiative feedback from a 16 Msun star forming in a cluster in one of our simulations results in the destruction of the main filament, the formation of an HII region, and the sweeping up of magnetic fields within an expanding shell of material at the edges of the HII region.}, added-at = {2016-08-18T23:48:04.000+0200}, author = {Klassen, Mikhail and Pudritz, Ralph E. and Kirk, Helen}, biburl = {https://www.bibsonomy.org/bibtex/21b8d60848502c0726650a7c9652dcdca/mvillagran}, description = {Filamentary flow and magnetic geometry in evolving cluster-forming molecular cloud clumps}, interhash = {0ca851b31d42d36de4eb65d71643af7b}, intrahash = {1b8d60848502c0726650a7c9652dcdca}, keywords = {DisPerSE Filaments Molecular}, note = {cite arxiv:1605.08835Comment: 26 pages, 19 figures, submitted to the MNRAS and revised in response to the referee report}, timestamp = {2016-08-18T23:48:04.000+0200}, title = {Filamentary flow and magnetic geometry in evolving cluster-forming molecular cloud clumps}, url = {http://arxiv.org/abs/1605.08835}, year = 2016 }