How do black holes 'leak' energy? Scientists have a new spin on the answer

We find that the saturated flux threading the BH has a weaker dependence on BH spin, compared to highly magnetized hot (geometrically thick) accretion flows. Also, we find that only a fraction (10%–70%) of the extracted BZ power is channeled into the jet, depending on the spin parameter. The remaining energy is potentially used to launch winds or contribute to the radiative output of the disk or corona. Our simulations reveal that the presence of a strong magnetic field enhances the radiative efficiency of the disk, making it more luminous than its weakly magnetized counterpart or the standard disk model. We attribute this excess luminosity primarily to the enhanced magnetic dissipation in the intra-ISCO region.

An earlier paper said [in 2012]:
Both shocked and shock-free flows have been studied in detail for rotating and counter-rotating accretion. Such a study has never been done in the literature before. We find that the energy extraction efficiency is low, about 0.1 per cent, and increases by a factor of 15 if the ram pressure is included. Such an efficiency is still much higher than the radiative efficiency of such optically thin flows.
https://academic.oup.com/mnrasl/article/421/1/L24/989131
 

Latest posts