The variability mechanisms from jetted AGNs are still under debate. Here the
damped random walk (DRW) model, implemented through Gaussian Processe (GPs), is
used to fit the $ZTF$ long-term optical light curves of 1684 $\gamma$-ray
emission jetted AGNs. This analysis yields one of the largest samples with
characteristic optical variability timescales for jetted AGNs. A single DRW
model from GPs can fit the optical light curve of most jetted AGNs
well/potentially well, while there are still some jetted AGNs whose light curve
can not be fitted well by a single DRW model. After the jet power, proxied by
gamma-ray luminosity, is introduced as a new parameter, new relationships among
intrinsic variability time scales, black hole mass and jet power are discovered
for efficient accretion AGNs ($\tau^{\rm in} \propto M_{\rm
BH}^{0.29^{+0.06}_{-0.06}}P_{\rm jet}^{-0.3^{+0.03}_{-0.03}}$ with scatter of
approximately 0.09~dex) and for inefficient accretion AGNs ($\tau^{\rm in}
\propto M_{\rm BH}^{0.06^{+0.07}_{-0.07}}P_{\rm jet}^{0.37^{+0.11}_{-0.11}}$
with scatter of approximately 0.14~dex), respectively. Our results support that
the optical variability of jetted AGNs with efficient accretion may originate
within the standard accretion disk at UV emitting radii similar to non-jetted
AGNs, and is directly related to the acceleration of shock in the jet and then
enhanced through the beaming effect in beamed AGNs. For the jetted AGNs with
inefficient accretion, the intrinsic timescale is consistent with the escape
timescale of electrons.

Dieser Artikel untersucht Zeitreisen und deren Auswirkungen.

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