التفاصيل البيبلوغرافية
| العنوان: |
How cold gas continuously entrains mass and momentum from a hot wind. |
| المؤلفون: |
Gronke, Max1 (AUTHOR) maxbg@ucsb.edu, Oh, S Peng1 (AUTHOR) |
| المصدر: |
Monthly Notices of the Royal Astronomical Society. 2/21/2020, Vol. 492 Issue 2, p1970-1990. 21p. |
| مصطلحات موضوعية: |
*KELVIN-Helmholtz instability, *COLD gases, *SPEED of sound, *WIND speed, *STAR formation, *GALACTIC halos, *MAGNETIC fields, *STELLAR winds |
| مستخلص: |
The existence of fast moving, cold gas ubiquitously observed in galactic winds is theoretically puzzling, since the destruction time of cold gas is much smaller than its acceleration time. In previous work, we showed that cold gas can accelerate to wind speeds and grow in mass if the radiative cooling time of mixed gas is shorter than the cloud destruction time. Here, we study this process in much more detail, and find remarkably robust cloud acceleration and growth in a wide variety of scenarios. Radiative cooling, rather than the Kelvin–Helmholtz instability, enables self-sustaining entrainment of hot gas on to the cloud via cooling-induced pressure gradients. Indeed, growth peaks when the cloud is almost co-moving. The entrainment velocity is of order the cold gas sound speed, and growth is accompanied by cloud pulsations. Growth is also robust to the background wind and initial cloud geometry. In an adiabatic Chevalier-Clegg type wind, for instance, the mass growth rate is constant. Although growth rates are similar with magnetic fields, cloud morphology changes dramatically, with low density, magnetically supported filaments, which have a small mass fraction but dominate by volume. This could bias absorption line observations. Cloud growth from entraining and cooling hot gas can potentially account for the cold gas content of the circumgalactic medium (CGM). It can also fuel star formation in the disc as cold gas recycled in a galactic fountain accretes and cools halo gas. We speculate that galaxy-scale simulations should converge in cold gas mass once cloud column densities of N ∼ 1018 cm−2 are resolved. [ABSTRACT FROM AUTHOR] |
| قاعدة البيانات: |
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