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

We perform a suite of simulations of cooling cores in clusters of galaxies inorder to investigate the effect of the recently discovered heat flux buoyancyinstability (HBI) on the evolution of cores. Our models follow the3-dimensional magnetohydrodynamics (MHD) of cooling cluster cores and capturethe effects of anisotropic heat conduction along the lines of magnetic field,but do not account for the cosmological setting of clusters or the presence ofAGN. Our model clusters can be divided into three groups according to theirfinal thermodynamical state: catastrophically collapsing cores, isothermalcores, and an intermediate group whose final state is determined by the initialconfiguration of magnetic field. Modeled cores that are reminiscent of realcluster cores show evolution towards thermal collapse on a time scale which isprolonged by a factor of ~2-10 compared with the zero-conduction cases. Theprincipal effect of the HBI is to re-orient field lines to be perpendicular tothe temperature gradient. Once the field has been wrapped up onto sphericalsurfaces surrounding the core, the core is insulated from further conductiveheating (with the effective thermal conduction suppressed to less than 1/100thof the Spitzer value) and proceeds to collapse. We speculate that, in realclusters, the central AGN and possibly mergers play the role of "stirrers,"periodically disrupting the azimuthal field structure and allowing thermalconduction to sporadically heat the core.

Simulations of MHD Instabilities in Intracluster Medium Including Anisotropic Thermal Conduction