Rimmed and rippled accretion disc models to explain AGN continuum lags

We propose a solution to the problem of accretion disc sizes in active galactic nuclei being larger when measured by reverberation mapping than predicted by theory. Considering the disc’s exposed-surface thickness profile H(r), our solution invokes a steep rim or rippled structures irradiated by the central lamp-post. We model the continuum lags and the faint and bright disc spectral energy distribution (SED) in the best-studied case NGC 5548 (black hole mass M_∙=7×10⁷M_⊙⁠, disc inclination i = 45°). With the lamp-post off, the faint-disc SED fixes a low accretion rate M˙≃0.0014 M_⊙yr⁻¹ and high prograde black hole spin a• ≃ 0.93, for which r_in=2GM_∙/c² and L_disc=0.25M˙c^2⁠. The bright-disc SED then requires a lamp-post luminosity L_LP≃5M˙c²/(1−A) for disc albedo A. Reprocessing on the thin disc with T ∝ r^−3/4 gives time lags τ ∝ λ^4/3 but three times smaller than observed. Introducing a steep H(r) rim, or multiple crests, near r ∼ 5 light days, reprocessing on the steep centre-facing slope increases temperatures from ∼1500 to ∼6000 K, and this increases optical lags to match the lag data. Most of the disc surface maintains the cooler T ∝ r^−3/4 profile that matches the SED. The bright lamp-post may be powered by magnetic links tapping the black hole spin. The steep rim occurs near the disc’s dust sublimation radius as in the ‘failed disc wind model for broad-line clouds’. Lens–Thirring torques aligning the disc and black hole spin may also raise a warp and associated waves. In both scenarios, the small density scale height implied by the inferred value of H(r) suggests possible marginal gravitational instability in the disc.