Winds Can "Blow Up" AGN Accretion Disk Sizes

TL;DR

This paper proposes that winds in AGN accretion disks can explain observed larger disk sizes and inter-band time lags, by modifying the temperature profile and emission contributions in the disk.

Contribution

The study introduces a wind-inclusive accretion disk model with a radially declining accretion rate, successfully explaining observed AGN disk sizes and variability features.

Findings

Model matches observed inter-band time lags of NGC 5548.

Wind effects lead to larger effective disk sizes.

The model explains variability in multiple AGN sources.

Abstract

Recent multi-band variability studies have revealed that active galactic nucleus (AGN) accretion disc sizes are generally larger than the predictions of the classical thin disc by a factor of $2\sim 3$. This hints at some missing key ingredient in the classical thin disc theory: here, we propose an accretion disc wind. For a given bolometric luminosity, in the outer part of an accretion disc, the effective temperature in the wind case is higher than that in the no-wind one; meanwhile, the radial temperature profile of the wind case is shallower than the no-wind one. In presence of winds, for a given band, blackbody emission from large radii can contribute more to the observed luminosity than the no-wind case. Therefore, the disc sizes of the wind case can be larger than those of the no-wind case. We demonstrate that a model with the accretion rate scaling as $\dot{M}_0 (R/R_{\mathrm{S}})^{\beta}$ (i.e., the accretion rate declines with decreasing radius due to winds) can match both the inter-band time lags and the spectral energy distribution of NGC 5548. Our model can also explain the inter-band time lags of other sources. Therefore, our model can help decipher current and future continuum reverberation mapping observations.