Relativistic Magnetized Jets: Power, Acceleration, and Collimation

          @misc{ scivideos_PIRSA:11120028,
            doi = {10.48660/11120028},
            url = {https://pirsa.org/11120028},
            author = {},
            keywords = {Strong Gravity},
            language = {en},
            title = {Relativistic Magnetized Jets: Power, Acceleration, and Collimation},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2011},
            month = {dec},
            note = {PIRSA:11120028 see, \url{https://scivideos.org/index.php/pirsa/11120028}}
          }
          

Abstract

After overviewing the fundamentals of magnetized relativistic jets production, I present the results of new global 3D general relativistic magnetohydrodynamic simulations of jet formation by black hole (BH) accretion systems. The simulations are designed to transport a large amount of magnetic flux to the center, more than the accreting gas can force into the BH. The excess magnetic flux remains outside the BH, impedes accretion, and leads to a magnetically arrested disc. We find powerful outflows. For a BH with spin parameter a = 0.5, the efficiency with which the accretion system generates outflowing energy in jets and winds is eta ~ 30%. For a = 0.99, we find eta ~ 140%, which means that more energy flows out of the BH than flows in. The only way this can happen is by extracting spin energy from the BH. Thus the a = 0.99 simulation represents an unambiguous demonstration, within an astrophysically plausible scenario, of the extraction of net energy from a spinning BH via the Penrose-Blandford-Znajek mechanism.