Formation of Interstellar Clouds: Parker Instability with Phase Transitions

Details Formation of Interstellar Clouds: Parker Instability with Phase Transitions Formation of Interstellar Clouds: Parker Instability with Phase Transitions

2009-01-07

arxiv.org/abs/0901.0914v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

11 pages, 7 figures, accepted for publication in MNRAS; high-resolution color figures may be found at https://netfiles.uiuc.

Scientific paper

We follow numerically the nonlinear evolution of the Parker instability in the presence of phase transitions from a warm to a cold HI interstellar medium in two spatial dimensions. The nonlinear evolution of the system favors modes that allow the magnetic field lines to cross the galactic plane. Cold HI clouds form with typical masses ~= 10^5 M_sun, mean densities ~= 20 cm^-3, mean magnetic field strengths ~= 4.3 muG (rms field strengths ~= 6.4 muG), mass-to-flux ratios ~= 0.1 - 0.3 relative to critical, temperatures ~= 50 K, (two-dimensional) turbulent velocity dispersions ~= 1.6 km s^-1, and separations ~= 500 pc, in agreement with observations. The maximum density and magnetic field strength are ~= 10^3 cm^-3 and ~= 20 muG, respectively. Approximately 60% of all HI mass is in the warm neutral medium. The cold neutral medium is arranged into sheet-like structures both perpendicular and parallel to the galactic plane, but it is also found almost everywhere in the galactic plane, with the density being highest in valleys of the magnetic field lines. `Cloudlets' also form whose physical properties are in quantitative agreement with those observed for such objects by Heiles (1967). The nonlinear phase of the evolution takes ~< 30 Myr, so that, if the instability is triggered by a nonlinear perturbation such as a spiral density shock wave, interstellar clouds can form within a time suggested by observations.

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