Groups and clusters will differ significantly from those predicted with the One immediateĬonsequence is that the colours and morphologies of satellite galaxies in To improve current semi-analytic models of galaxy formation. Stripping of both observed and cosmologically-simulated galaxies and as a way Has several interesting applications, including modelling the ram pressure the pressure exerted by the hot and dense intracluster medium (ICM) on galaxies moving at high velocity within the cluster gravitational potential well, is a key process able to remove their interstellar medium (ISM) and quench their activity of star formation. Under-predicts the stripping following pericentric passage). Among these, ram pressure stripping, i.e. The group or cluster into which it is falling (in which case the model The orbit of the galaxy is highly non-radial and its mass exceeds about 10% of are defined by stellar mass and star formation rates to compare the star. outermost gas layers of galaxies in nearby and/or low-mass galaxy clusters. Abstract: We study galaxies undergoing ram pressure stripping in the Virgo. The one exception involves unlikely systems where Ram-pressure stripping by the gaseous intracluster medium has been proposed. The model reproduces the results of the simulations to within approximately 10%Īt almost all times for all the orbits, mass ratios, and galaxy structural That stripping is not instantaneous but occurs on a characteristic timescale. is ISM and that the mean mass density (usually dominated by stars) of the disk is. Gas distribution (as opposed to a face-on cold disk) and takes into account 12.5.3 Ram-Pressure Stripping When a galaxy moves through the. Gott (1972), except that it is appropriate for the case of a spherical (hot) The model is analogous to the original formulation of Gunn &
Simple analytic model that describes the stripping seen in the simulations Galactic halo gas can remain in place after 10 Gyr. Typical structural and orbital parameters, we find that ~30% of the initial hot Orbit, total galaxy mass, and galaxy structural properties is explored. We call the subsamples out of HIFLUCGS and RXGCC the high-mass and low-mass cluster samples respectively in the following analysis. We solved the model equations numerically in two dimensions and extended the range of parameters beyond the range. Our equations differ from those of Gaetz, Salpeter, and Shaviv in the treatment of the motion of stars in the galaxy. Study the ram pressure stripping of the hot gaseous halos of galaxies as theyįall into massive groups and clusters. We examine the physical assumptions and the basic hydrodynamic equations of the ram pressure stripping model for elliptical galaxies in clusters of galaxies.
RAM PRESSURE STRIPPING MASS PDF
Balogh (2), Tom Theuns (1,3) ((1) ICC, Durham, (2) Waterloo, (3) Antwerp) Download PDF Abstract: We use a large suite of carefully controlled full hydrodynamic simulations to
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