%0 Generic %1 girichidis2015launching %A Girichidis, Philipp %A Naab, Thorsten %A Walch, Stefanie %A Hanasz, Michal %A Mac Low, Mordecai-Mark %A Ostriker, Jeremiah P. %A Gatto, Andrea %A Peters, Thomas %A Wünsch, Richard %A Glover, Simon C. O. %A Klessen, Ralf S. %A Clark, Paul C. %A Baczynski, Christian %D 2015 %K cosmic launching outflows ray %T Launching Cosmic ray-driven Outflows from the magnetized interstellar medium %U http://arxiv.org/abs/1509.07247 %X We present a hydrodynamical simulation of the turbulent, magnetized, supernova-driven interstellar medium (ISM) in a stratified box that dynamically couples the injection and evolution of cosmic rays (CRs) and a self-consistent evolution of the chemical composition. CRs are treated as a relativistic fluid in the advection-diffusion approximation. The thermodynamic evolution of the gas is computed using a chemical network that follows the abundances of H+, H, H2, CO, C+, and free electrons and includes (self-)shielding of the gas and dust. We find that CRs perceptibly thicken the disk with the heights of 90% (70%) enclosed mass reaching ~1.5 kpc (~0.2 kpc). The simulations indicate that CRs alone can launch and sustain strong outflows of atomic and ionized gas with mass loading factors of order unity, even in solar neighbourhood conditions and with a CR energy injection per supernova (SN) of 10^50 erg, 10% of the fiducial thermal energy of a SN. The CR-driven outflows have moderate launching velocities close to the midplane (~100 km/s) and are denser (\rho~1e-24 - 1e-26 g/cm^3), smoother and colder than the (thermal) SN-driven winds. The simulations support the importance of CRs for setting the vertical structure of the disk as well as the driving of winds.

@misc{girichidis2015launching, abstract = {We present a hydrodynamical simulation of the turbulent, magnetized, supernova-driven interstellar medium (ISM) in a stratified box that dynamically couples the injection and evolution of cosmic rays (CRs) and a self-consistent evolution of the chemical composition. CRs are treated as a relativistic fluid in the advection-diffusion approximation. The thermodynamic evolution of the gas is computed using a chemical network that follows the abundances of H+, H, H2, CO, C+, and free electrons and includes (self-)shielding of the gas and dust. We find that CRs perceptibly thicken the disk with the heights of 90% (70%) enclosed mass reaching ~1.5 kpc (~0.2 kpc). The simulations indicate that CRs alone can launch and sustain strong outflows of atomic and ionized gas with mass loading factors of order unity, even in solar neighbourhood conditions and with a CR energy injection per supernova (SN) of 10^50 erg, 10% of the fiducial thermal energy of a SN. The CR-driven outflows have moderate launching velocities close to the midplane (~100 km/s) and are denser (\rho~1e-24 - 1e-26 g/cm^3), smoother and colder than the (thermal) SN-driven winds. The simulations support the importance of CRs for setting the vertical structure of the disk as well as the driving of winds.}, added-at = {2015-09-25T09:50:28.000+0200}, author = {Girichidis, Philipp and Naab, Thorsten and Walch, Stefanie and Hanasz, Michal and Mac Low, Mordecai-Mark and Ostriker, Jeremiah P. and Gatto, Andrea and Peters, Thomas and Wünsch, Richard and Glover, Simon C. O. and Klessen, Ralf S. and Clark, Paul C. and Baczynski, Christian}, biburl = {https://www.bibsonomy.org/bibtex/2f6694cecd37fcfd8b226cf0eb6a36cf1/miki}, description = {[1509.07247] Launching Cosmic ray-driven Outflows from the magnetized interstellar medium}, interhash = {ee404493e46c815c14863cf694a18ac5}, intrahash = {f6694cecd37fcfd8b226cf0eb6a36cf1}, keywords = {cosmic launching outflows ray}, note = {cite arxiv:1509.07247Comment: 7 pages, 5 figures, submitted, comments welcome}, timestamp = {2015-09-25T09:50:28.000+0200}, title = {Launching Cosmic ray-driven Outflows from the magnetized interstellar medium}, url = {http://arxiv.org/abs/1509.07247}, year = 2015 }