Galaxies living in rich environments are suffering different perturbations able to drastically
affect their evolution. Among these, ram pressure strip**, ie the pressure exerted by the …

Star-forming gas clouds are strongly magnetized, and their ionization fractions are high
enough to place them close to the regime of ideal magnetohydrodyamics on all but the …

dense shell formation rate) and energy balance (supernova shock input= radiation loss)
determine the density and temperature of the hot medium with (n, T)=(1O_2. 5, lO~. 7) being …

Interstellar bubbles. II - Structure and evolution ADS Classic is now deprecated. It will be
completely retired in October 2019. This page will automatically redirect to the new ADS …

This paper describes the open-source code Enzo, which uses block-structured adaptive
mesh refinement to provide high spatial and temporal resolution for modeling astrophysical …

The interaction of a uniformly expanding gas with a stationary ambient medium is studied in
the case where the expanding matter has a power-law density profile (ρ∝ rn), as well as the …

We investigate the physical mechanisms that shape the luminosity function of galaxies in
hierarchical clustering models. Beginning with the mass function of dark matter halos in the …

Increasingly, uncertainties in predictions from galaxy formation simulations (at sub-Milky
Way masses) are dominated by uncertainties in stellar evolution inputs. In this paper, we …

We present a novel analytic framework to model the steady-state structure of multiphase
galactic winds comprised of a hot, volume-filling component and a cold, clumpy component …

The interstellar medium (ISM) is inhomogeneous, with clouds of various temperatures and
densities embedded in a tenuous intercloud medium. Shocks propagating through the ISM …