2009/02/28 by James Binney, J. Binney, Carlo Nipoti +3 · 123 citations
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Corona (planetary geology) #Galactic corona #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Instability #Mechanics #Milky Way #Physics #Thermal #Venus #astro-ph.GA
paper · pdf · doi:10.1111/j.1365-2966.2009.15113.x
published in Monthly Notices of the Royal Astronomical Society 397(4), 1804-1815 (Oxford University Press) · MNRAS, accepted. 13 pages, 8 figures. Added discussion with respect to submitted version
arxiv created 2009/05/20 · openalex publication_date 2009/07/28 · arxiv updated 2015/05/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We examine the proposal that the H i‘high-velocity’ clouds (HVCs) surrounding the Milky Way and other disc galaxies form by condensation of the hot galactic corona via thermal instability. Under the assumption that the galactic corona is well represented by a non-rotating, stratified atmosphere, we find that for this formation mechanism to work the corona must have an almost perfectly flat entropy profile. In all other cases, the growth of thermal perturbations is suppressed by a combination of buoyancy and thermal conduction. Even if the entropy profile were nearly flat, cold clouds with sizes smaller than 10 kpc could form in the corona of the Milky Way only at radii larger than 100 kpc, in contradiction with the determined distances of the largest HVC complexes. Clouds with sizes of a few kpc can form in the inner halo only in low-mass systems. We conclude that unless even slow rotation qualitatively changes the dynamics of a corona, thermal instability is unlikely to be a viable mechanism for formation of cold clouds around disc galaxies.