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

Dynamics of clumps within a magnetized advection dominated accretion flow isinvestigated by solving the collisionless Boltzmann equation and consideringthe drag force due to the relative velocity between the clumps and the gas.Toroidal component of the magnetic field is assumed to be dominant. Dynamicalproperties of the hot gaseous component such as the radial and the rotationalvelocities are affected by the magnetic effects, and so, drag force variesdepending on the strength of magnetic field and the velocity dispersion of theclumps is then modified significantly. We show that when magnetic pressure isless than the gas pressure, the root of the averaged radial velocity square ofthe clumps decreases at the inner parts of the hot flow and increases slightlyat its outer edge.

Dynamics of clumps embedded in a hot accretion flow with toroidal magnetic field