![]() ![]() ![]() In cases in which the gas is not completely stripped, the propagation of possible galactic wind may be influenced by the disturbed distribution of the interstellar matter. This poses an interesting question on the aspect of the descents and, more in general, on the morphological evolution of dwarf galaxies. Despite the low values of the ram pressure, some dwarf galaxies can be completely stripped after 100-200 Myr. It turns out that this last parameter plays a role only when the gas pressure in the galactic centre is comparable to the ram pressure. The nonlinear coupling that develops between the fluid and solid materi-als dictates that a detailed mathemati-cal description of the. We study the ram pressure effects as a function of several parameters such as galactic mass and velocity, ambient gas density and the angle between the galactic plane and the direction of motion. Hydrodynamic ram is a phenomenon that the kinetic energy of a high-speed impact projectile is converted into highly destructive pressure waves in a fluid-filled environment, which can cause the catastrophic structural damage 1. sion of the physical effects through the interaction of the projectile, the fluid, and the structure as well as the abnormally excessive structural dam-age that results from this fluid-solid interaction (FSI). We extend over previous investigations by considering flattened, rotating dwarf galaxies subject to ram pressures typical of poor galaxy groups. ![]() Analogous studies on this subject usually deal with much higher ram pressures, typical of galaxy clusters, or mild ram pressure due to the gas halo of the massive galactic companions. We present three-dimensional hydrodynamic simulations of ram pressure stripping in dwarf galaxies. ![]()
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