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

Magellanic spiral galaxies are a class of one-armed systems that oftenexhibit an offset stellar bar, and are rarely found around massive spiralgalaxies. Using a set of N-body and hydrodynamic simulations we consider adwarf-dwarf galaxy interaction as the driving mechanism for the formation ofthis peculiar class of systems. We investigate here the relation between thedynamical, stellar and gaseous disk center and the bar. In all our simulationsthe bar center always coincides with the dynamical center, while the stellardisk becomes highly asymmetric during the encounter causing the photometriccenter of the Magellanic galaxy disk to become mismatched with both the bar andthe dynamical center. The disk asymmetries persist for almost 2 Gyrs, the timethat it takes for the disk to be re-centered with the bar, and well after thecompanion has passed. This explains the nature of the offset bar found in manyMagellanic-type galaxies, including the Large Magellanic Cloud (LMC) and NGC3906. In particular, these results, once applied to the LMC, suggest that thedynamical center should reside in the bar center instead of the HI center aspreviously assumed, pointing to a variation in the current estimate of thenorth component of the LMC proper motion.

Tidally Induced Offset Disks in Magellanic Spiral Galaxies