Launching cosmic-ray-driven outflows from the magnetized interstellar medium

• Verfasst von: Girichidis, Philipp [VerfasserIn]
• Verfasst von: Naab, Thorsten [VerfasserIn]
• Verfasst von: Walch, Stefanie [VerfasserIn]
• Verfasst von: Hanasz, Michal [VerfasserIn]
• Verfasst von: Mac Low, Mordecai-Mark [VerfasserIn]
• Verfasst von: Ostriker, Jeremiah P. [VerfasserIn]
• Verfasst von: Gatto, Andrea [VerfasserIn]
• Verfasst von: Peters, Thomas [VerfasserIn]
• Verfasst von: Wünsch, Richard [VerfasserIn]
• Verfasst von: Glover, Simon [VerfasserIn]
• Verfasst von: Klessen, Ralf S. [VerfasserIn]
• Verfasst von: Clark, Paul C. [VerfasserIn]
• Verfasst von: Baczynski, Christian [VerfasserIn]
• Titel: Launching cosmic-ray-driven outflows from the magnetized interstellar medium
• Verf.angabe: Philipp Girichidis, Thorsten Naab, Stefanie Walch, Michal Hanasz, Mordecai-Mark Mac Low, Jeremiah P. Ostriker, Andrea Gatto, Thomas Peters, Richard Wünsch, Simon C. O. Glover, Ralf S. Klessen, Paul C. Clark, Christian Baczynski
• E-Jahr: 2016
• Jahr: 6 Jan 2016
• Umfang: 7 S.
• Fussnoten: Gesehen am 10.06.2020
• Titel Quelle: Enthalten in: The astrophysical journal / 2
• Ort Quelle: London : Institute of Physics Publ., 1995
• Jahr Quelle: 2016
• Band/Heft Quelle: 816(2016,2) Artikel-Nummer L19, 7 Seiten
• ISSN Quelle: 2041-8213
• DOI: doi:10.3847/2041-8205/816/2/L19
• Datenträger: Online-Ressource
• Sprache: eng
• Sach-SW: Astrophysics - Astrophysics of Galaxies
• K10plus-PPN: 1700345834

Abstract

We present a hydrodynamical simulation of the turbulent, magnetized, supernova (SN)-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 neighborhood conditions and with a CR energy injection per SN of 10^50 erg, 10% of the fiducial thermal energy of an 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.