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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

(abridged) Ram pressure can remove significant amounts of gas from galaxiesin clusters, and thus has a large impact on the evolution of cluster galaxies.Recent observations have shown that key properties of ram pressure strippedtails of galaxies are in conflict with predictions by simulations. To increasethe realism of existing simulations, we simulated for the first time a diskgalaxy exposed to a uniformly magnetized wind including radiative cooling andself-gravity of the gas. We find that B-fields have a strong effect on themorphology of the gas in the tail of the galaxy. While in the pure hydro casethe tail is very clumpy, the MHD case shows very filamentary structures in thetail. The filaments can be strongly supported by magnetic pressure and, whenthis is the case, the B-field vectors tend to be aligned with the filaments.The ram pressure stripping may lead to the formation of magnetized densitytails that appear as bifurcated in the plane of the sky and resemble the doubletails observed in ESO 137-001 and ESO 137-002. Such tails can be formed under avariety of situations, both for the disks oriented face-on with respect to theICM wind and for the tilted ones. While this bifurcation is due to the generictendency for the B-fields to produce very filamentary tail morphology, the tailproperties are further shaped by the combination of the B-field orientation andthe sliding of the field past the disk surface exposed to the wind. Magneticdraping does not strongly change the rate of gas stripping. For a face-ongalaxy, the field tends to reduce the amount of stripping compared to the purehydro case, and is associated with the formation of a magnetic draping layer onthe side of the galaxy exposed to the ICM wind. For significantly tilted disks,the stripping rate may be enhanced by the ``scraping'' of the disk surface bythe B-fields sliding past the ISM/ICM interface.

Impact of magnetic fields on ram pressure stripping in disk galaxies