Charged Black holes in AdS5×S5 suffer from superradiant instabilities over a range of energies. Hairy black hole solutions (constructed within gauged supergravity) have previously been proposed as endpoints to this instability. We demonstrate that these hairy black holes are themselves unstable to the emission of large dual giant gravitons. We propose that the endpoint to this instability is given by Dual Dressed Black Holes (DDBH)s; configurations consisting of one, two, or three very large dual giant gravitons surrounding a core AdS black hole with one, two, or three SO(6) chemical potentials equal to unity. The dual giants each live at AdS radial coordinates of order √N and each carry charge of order N2. The large separation makes DDBHs a very weakly interacting mix of their components and allows for a simple computation of their thermodynamics. We conjecture that DDBHs dominate the phase diagram of N=4 Yang-Mills over a range of energies around the BPS plane, and provide an explicit construction of this phase diagram, briefly discussing the interplay with supersymmetry. We develop the quantum description of dual giants around black hole backgrounds and explicitly verify that DDBHs are stable to potential tunneling instabilities, precisely when the chemical potentials of the core black holes equal unity. We also construct the 10-dimensional DDBH bulk solutions.
Author indications on fulfilling journal expectations
Provide a novel and synergetic link between different research areas.
Open a new pathway in an existing or a new research direction, with clear potential for multi-pronged follow-up work
Detail a groundbreaking theoretical/experimental/computational discovery
Present a breakthrough on a previously-identified and long-standing research stumbling block
Author comments upon resubmission
In the resubmitted version, we made some changes to address the comments made by the referees.
List of changes
1. In the revised version we changed the term ⊇rgravitysolutions’→bulk solutions’ all through the paper (including in the abstract). 2. We have added the new footnote number 22 . This footnote reads "Gauged supergravity is believed to form a consistent truncation of the full 10 d supergravity in the following sense. If we decompose 10 d supergravity into 5d fields, denote those fields that lie in gauged supergravity a a type fields, and those fields that lie outside gauged supergravity as b type fields, then it is believed that all couplings between a and b type fields are of quadratic or higher order in b. As a consequence, a solution of gauged supergravity never sources b type fields including all those dual to Tr(Zn) for all n≥3. . 3. We have added footnote 39 which reads "The analysis presented in this subsection applies whenever mN is small. This is certainly the case when m is of order unity, as assumed in the main text in the rest of this subsection. However it is also the case when m=ζN with ζ≪1 (see \S ??? for a discussion of bulk solutions corresponding to this case). The probe analysis of the rest of this section (see (???)) tells us that the reduction of flux at the centre of the black hole results in a fractional lowering of entropy of order O(ζ). The analysis of \S ??? then tells us that interaction effects correct probe estimates at order ζd4=O(ζ3), and so are negligible at small ζ. This discussion strongly suggests that the solutions described in this paper maximize entropy locally (in configuration space). We emphasize that nothing presented in this paper rules out the possible existence of new nonlinear solutions of supergravity that have even higher entropy than the solutions presented in this paper. For instance, we cannot rule out the possibility that thermodynamics is dominated by a new nonlinear solution - which can be, in some sense, thought of as `ζ of order unity'." 4. We have added a footnote 10 which reads " As we explain in \S ???, this instability involves tunneling through a barrier. Consequently, it is perhaps more accurate to say that black holes with μi>1 are metastable in the microcanonical ensemble. We expect the same black holes to have a simpler `roll down the hill' instability in the grand canonical ensemble (see \S ???). 5. We have added 4 new figures, Figs 2, 3, 11 and 12. 6. We have rewritten parts of section 5.1 to make this section clearer and easier to read. 7. We fixed various typos.
