Viscously Spreading Accretion Disks around Black Holes: Implications for TDEs, LFBOTs and other Transients

TL;DR

This paper introduces a comprehensive time-dependent model of viscously spreading accretion disks around black holes, explaining late-time emissions in TDEs and LFBOTs, and highlighting the importance of disk physics and irradiation effects.

Contribution

It generalizes previous models by including outflows, non-conservation effects, irradiation, and various viscous stress models, providing new insights into late-time emissions in TDEs and LFBOTs.

Findings

Late-time plateaus in TDEs can be explained by disks with a large spread in angular momentum.

Viscous spreading on year timescales is not necessary to explain observations.

Magnetically dominated disks better match TDE plateau luminosities than radiation pressure dominated thin disks.

Abstract

We present a simple time-dependent model of viscously spreading accretion disks around black holes (BHs) with masses between $10-10^8M_\odot$. We apply the results to observations of late-time emission in tidal disruption events (TDEs) and luminous fast blue optical transients (LFBOT) such as AT2018cow. Our model generalizes previous work by incorporating outflows during super-Eddington accretion, non-conservation of mass and angular momentum in TDE circularization, irradiation of the outer disk by the inner accretion flow, and a range of viscous stress models. We show that many late-time plateaus in TDEs can be explained by disks formed with a large spread in angular momentum due to redistribution during circularization. Viscous spreading on year timescales is not required, although it is also compatible with the data. The collapse of radiation pressure dominated thin disks to the stable gas-pressure dominated phase greatly underpredicts TDE plateau luminosities, strongly favoring thermally stable magnetically dominated disk models. Irradiation of the outer disk in TDEs due to misalignment of the stellar orbit and black hole spin increases plateau luminosities and durations by factors of a few. Continued study of late-time TDE emission provides a unique opportunity to constrain the physics of disk formation and circularization, disk warps, angular momentum transport, and other poorly understood aspects of disk physics. The models we develop can also explain the late-time optical-UV emission in the LFBOT AT2018cow for BH masses of ~$10-100M_\odot$. The faint X-ray emission at late times in AT2018cow is likely due to ongoing absorption. Our models predict that late-time X-rays should eventually be detectable again, and that HST/JWST observations of AT2018cow may detect a break in the SED at near-IR-optical wavelengths, providing a powerful probe of outer accretion disk thermodynamics.