Research Library | Digital Repository

How do velocity structure functions trace gas dynamics in simulated molecular clouds?

Show simple item record Chira, Roxana-Adela Ibáñez-Mejía, Juan C. Mac Low, Mordecai-Mark Henning, Thomas 2018-08-08T20:59:24Z 2018-08-08T20:59:24Z 2018-07-27
dc.description.abstract In Chira et al. (subm.), we investigate the time evolution of gas dynamics within simulated molecular clouds, as well as how velocity structure functions trace the dominating driving sources of turbulence. The molecular clouds are formed self-consistently within kiloparsec-scale numerical simulations of the interstellar medium that include self-gravity, magnetic fields, supernovae- driven turbulence, and radiative heating and cooling. Here, we provide the underlying data for the analysis and plots presented in the paper submitted to Astronomy & Astrophysics. The simulations are run using an implementation of the Flash code. We present data for each of the, in total, 160 timesteps in HDF5 format, the final velocity structure functions as functions of lag and time. Note that due to technical problems we are currently able to offer the raw data for those simulations that resolve the local Jeans length with 4 cells only. We will upload the higher Jeans-resolved data as soon as possible. en_US
dc.rights Attribution-NonCommercial-ShareAlike 3.0 United States *
dc.rights.uri *
dc.subject Turbulence
dc.subject ISM: kinematics and dynamics
dc.subject ISM: structure
dc.subject ISM: clouds
dc.title How do velocity structure functions trace gas dynamics in simulated molecular clouds? en_US

Files in this item

The following license files are associated with this item:

This item appears in the following Collection(s)

Show simple item record

Attribution-NonCommercial-ShareAlike 3.0 United States Except where otherwise noted, this item's license is described as Attribution-NonCommercial-ShareAlike 3.0 United States

Search Entire Repository

Advanced Search


My Account