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

Using long-duration general relativistic magnetohydrodynamic simulations ofradiatively inefficient accretion discs, the energy, momentum and mass outflowrates from such systems are estimated. Outflows occur via two fairly distinctmodes: a relativistic jet and a sub-relativistic wind. The jet power dependsstrongly on the black hole spin and on the magnetic flux at the horizon. Unlessthese are very small, the energy output in the jet dominates over that in thewind. For a rapidly spinning black hole accreting in the magnetically arrestedlimit, it is confirmed that jet power exceeds the total rate of accretion ofrest mass energy. However, because of strong collimation, the jet probably doesnot have a significant feedback effect on its immediate surroundings. The powerin the wind is more modest and shows a weaker dependence on black hole spin andmagnetic flux. Nevertheless, because the wind subtends a large solid angle, itis expected to provide efficient feedback on a wide range of scales inside thehost galaxy. Empirical formulae are obtained for the energy and momentumoutflow rates in the jet and the wind.

Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes