The Ultraviolet/optical variability of steep-spectrum radio quasars: the change in accretion rate ?

TL;DR

This study investigates UV/optical variability in steep-spectrum radio quasars, finding that changes in accretion rate of the disk likely drive the observed flux variations, with jet emission also playing a role.

Contribution

It demonstrates that the UV/optical variability in SSRQs can be explained by a standard accretion disk model with variable accretion rates, providing new insights into their variability mechanisms.

Findings

Flux-flux diagrams are well described by accretion rate changes.

Variable accretion rate models fit the data with reasonable parameters.

Jet emission can also reproduce variability but requires less plausible parameters.

Abstract

Context. The steep-spectrum radio quasars (SSRQs) are powerful radio sources, with thermal emission from accretion disk and jet nonthermal emission likely both contributing in the Ultraviolet (UV)/optical luminosity, however the former may play a dominant role. While the UV/optical variability of SSRQs has been poorly studied, little is known on the mechanism of their variability. Aims. We investigate the mechanism of the UV/optical variability of SSRQs. Methods. A sample of eighteen SSRQs has been established in SDSS Stripe 82 region in our previous works, in which the flux and spectral variability have been studied. In this work, we construct the flux-flux diagram using SDSS u and i multi-epoch data for these eighteen SSRQs. The standard accretion disk model is used to fit the flux-flux variations, in order to explore the variability mechanism. Results. The model fit to flux-flux diagram are tuned with fixed black hole mass and varying accretion rate. We found that the flux-flux diagram of all our SSRQs can be qualitatively described by the standard accretion disk model with change of the accretion rate. Although non-thermal jet power-law emission can also qualitatively reproduce the variability, the reasonable accretion rates and black hole masses required to fit the flux-flux variations suggest that a disk emission with variable accretion rate is a plausible description of the data.