English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The influence of a time-varying ram pressure on spiral galaxies in clustersis explored with a new simulation method based on the N-body SPH/tree codeGADGET. We have adapted the code to describe the interaction of two differentgas phases, the diffuse hot intracluster medium (ICM) and the denser and colderinterstellar medium (ISM). Both the ICM and ISM components are introduced asSPH particles. As a galaxy arrives on a highly radial orbit from outskirts tocluster center, it crosses the ICM density peak and experiences a time-varyingwind. Depending on the duration and intensity of the ISM-ICM interaction, earlyand late type galaxies in galaxy clusters with either a large or small ICMdistribution are found to show different stripping efficiencies, amounts ofreaccretion of the extra-planar ISM, and final masses. We compare the numericalresults with analytical approximations of different complexity and indicate thelimits of the Gunn & Gott simple stripping formula. Our investigationsemphasize the role of the galactic orbital history to the stripping amount. Wediscuss the contribution of ram pressure stripping to the origin of the ICM andits metallicity. We propose gas accumulations like tails, filaments, or ripplesto be responsible for stripping in regions with low overall ICM occurrence.

Gas stripping in galaxy clusters: a new SPH simulation approach