Ram Pressure Stripping of Spiral Galaxies in Clusters

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dc.creatorAbadi, Mario G.
dc.creatorMoore, Ben
dc.creatorBower, Richard G.
dc.date1999-03-29
dc.date1999-03-31
dc.date.accessioned2026-07-07T10:31:50Z
dc.date.available2026-07-07T10:31:50Z
dc.descriptionWe use 3-dimensional SPH/N-BODY simulations to study ram pressure stripping of gas from spiral galaxies orbiting in clusters. We find that the analytic expectation of Gunn & Gott (1972) relating the gravitational restoring force provided by the disk to the ram pressure force, provides a good approximation to the radius that gas will be stripped from a galaxy. However, at small radii it is also important to consider the potential provided by the bulge component. A spiral galaxy passing through the core of a rich cluster such as Coma, will have its gaseous disk truncated to $\sim 4$ kpc, thus losing $\sim 80%$ of its diffuse gas mass. The timescale for this to occur is a fraction of a crossing time $\sim 10^7$ years. Galaxies orbiting within poorer clusters, or inclined to the direction of motion through the intra-cluster medium will lose significantly less gas. We conclude that ram-pressure alone is insufficient to account for the rapid and widespread truncation of star-formation observed in cluster galaxies, or the morphological transformation of Sab's to S0's that is necessary to explain the Butcher-Oemler effect.
dc.description8 pages, 7 figures, to be published in MNRAS. Levels added/corrected on figures 3, 4 and 5
dc.identifierhttps://arxiv.org/abs/astro-ph/9903436
dc.identifierhttp://arxiv.org/abs/astro-ph/9903436
dc.identifierMon.Not.Roy.Astron.Soc.308:947-954,1999
dc.identifierdoi:10.1046/j.1365-8711.1999.02715.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/178554
dc.subjectAstrophysics
dc.titleRam Pressure Stripping of Spiral Galaxies in Clusters
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