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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Based on a comparison of dynamical models with observations of theinterstellar gas in 6 Virgo cluster spiral galaxies a first complete rampressure stripping time sequence has been established. The observationalcharacteristics of the different stages of ram pressure stripping arepresented. The dynamical models yield the 3D velocity vectors of the galaxies,peak ram pressures, and times to peak ram pressure. In the case of a smooth,static, and spherical intracluster medium, peak ram pressure occurs during thegalaxy's closest approach to the cluster center, i.e. when the galaxy'svelocity vector is perpendicular to its distance vector from the cluster center(M 87). Assuming this condition the galaxy's present line-of-sight distance andits 3D position during peak ram pressure can be calculated. The linear orbitalsegments derived in this way together with the intracluster medium densitydistribution derived from X-ray observations give estimates of the ram pressurethat are on average a factor of 2 higher than derived from the dynamicalsimulations for NGC 4501, NGC 4330, and NGC 4569. Resolving this discrepancywould require either a 2 times higher intracluster medium density than derivedfrom X-ray observations, or a 2 times higher stripping efficiency than assumedby the dynamical models. Compared to NGC 4501, NGC 4330, and NGC 4569, NGC 4388requires a still 2 times higher local intracluster medium density or adirection which is moderately different from that derived from the dynamicalmodel. A possible scenario for the dynamical evolution of NGC 4438 and M 86within the Virgo cluster is presented.

A holistic view on ram pressure stripping in the Virgo cluster - The first complete model-based time sequence