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If some of the n 's H tend to in"nity, the solutions approach the RN (for "0) or charged dilaton (for O0) black hole solutions. One of the new features is that when some of the w 's vanish identically, the U(1) charges arise. H The non-Abelian baldness theorem hence does not generalize to higher gauge groups. 59) w "0, the solutions for w show the usual nodal structure. 62), there is a magne tic charge P"(3 for all n . 2M/r#P/r#O(1/r). For higher gauge groups one can obtain in this way a variety of charged solutions, in particular, solutions with an electric charge (for a more general ansatz for the gauge "eld).
8) 1 r . 10) Here M coincides with the mass of the RN black hole with unit charge. The following approxima tion is very good for n52 and r51: M (r )+M (see Fig. 8). This is due to the fact that for large L values of n the amplitude w oscillates in a small vicinity of zero. S. V. Galt'sov / Physics Reports 319 (1999) 1}83 Fig. 8. The ADM mass M (r ) and the temperature screening coe$cient (r ) versus the event horizon radius. For n"0 L L solutions are Schwarzschild. Eq. 8) is then close to unity, while metric is approximately RN.
This shows that the non-Abeian black holes generically do not possess inner horizons [128,130,58,57] and therefore have a spacelike singularity, as suggested by the strong cosmic censorship hypothesis. 2) in the vicinity of the singularity at r"0. One "nds three distinct types of local solutions, but none of them are generic. S. V. Galt'sov / Physics Reports 319 (1999) 1}83 with arbitrary m and b. Since the inner horizon is generically absent, a solution of this type should match the one propagating inwards from r .