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tokens: of the initial rotational energy. Other energies increase the irreducible mass of the BH. For a • (0) = 0.5, M • = 0.98 M • (0), or 2% of the initial mass can be used to power a GRB. 10 10 Atteia et al. ( 2017 ) found the maximum isotropic energy of GRBs when they studied the GRB energy distribution within redshifts z = 1–5. Jet break measurements are needed to derive the beaming-corrected energy, which can be compared with our model predictions. As the magnetic field on the BH is supported by the surrounding disk, there are some relations between B • and . In a hyperaccreting flow in a GRB, it is possible that a magnetic flux is accumulated near the BH horizon. Considering the balance between the magnetic pressure on the horizon and the ram pressure of the innermost part of the accretion flow (e.g., Moderski et al. 1997 ), one can estimate the magnetic field strength threading the BH horizon , where is the radius of the BH horizon. One thus hasInserting it into Equation ( 31 ), we obtain the magnetic power and torque as a function of the mass accretion rate and BH spin, i.e., where . It is found that X (0) = 1/6 and X (1) = π − 2. Both neutrino-annihilation and magnetic powers depend on the disk mass accretion. In Figure 3 , we present the BZ power as a function of accretion rate for different BH spins and compare it with the neutrino-annihilation power. We find that (1) the magnetic power is much greater than the neutrino-annihilation power for a moderate to high-spin BH, (2) the neutrino-annihilation power dominates over the BZ power for BHs with a very small spin at high accretion rates, and (3) compared with the magnetic power, is much more sensitive to the mass accretion rate . Therefore, if the disk accretion rate is variable, the jet driven by the neutrino-annihilation process should be highly variable. However, the MHD jet is usually subject to instabilities, such as kink instability (Wang et al. 2006 ) and magnetic reconnection (e.g., the Internal-Collision induced Magnetic Reconnection and Turbulence, ICMART, in Zhang Yan 2011 ). These MHD processes will add complexity to the GRB light curves. Figure 3. Magnetic power as a function of accretion rate for different BH spins, a • = 0.01 (thick red solid line) and 0.99 (thick blue solid lines). The dashed lines show the neutrino-annihilation power calculated with Equation ( 22 ) for a • = 0.01 (red dashed line) and 0.99 (blue dashed line). The thin blue line is produced with the analytic expression of Tchekhovskoy et al. ( 2011 ) for a • = 0.99, where the average magnetic flux and κ = 0.044 are taken based on the numerical simulation Model A0.99f. In the magnetic model, baryons from the disk will be suppressed by the strong magnetic field lines. For , the baryon-loading rate for the BZ-driven jet is (Paper I )For , the dependence of on will be . In Equation ( 39 ), f p is the fraction of protons and r z is the distance from the BH in the jet direction, which is normalized to 10 11 cm.