  Recently, a black hole model in loop quantum gravity has been proposed by
Lewandowski, Ma, Yang and Zhang (Phys. Rev. Lett. \textbf{130}, 101501 (2023)).
The metric tensor of the quantum black hole (QBH) is a suitably modified
Schwarzschild one. In this paper, we calculate the radius of light ring and
obtain the linear approximation of it with respect to the quantum correction
parameter $\alpha$: $r_{l} \simeq 3 M - \frac{\alpha}{9 M}$. We then assume the
QBH is backlit by a large, distant plane of uniform, isotropic emission and
calculate the radius of the black hole shadow and its linear approximation:
$r_{s} = 3 \sqrt{3} M - \frac{\alpha}{6 \left(\sqrt{3} M\right)}$. We also
consider the photon ring structures in the shadow when the impact parameter $b$
of the photon approaches to a critical impact parameter $b_{\textrm{c}}$, and
obtain a formula for estimating the deflection angle, which is
$\varphi_{\textrm{def}} = - \frac{\sqrt{2}}{\omega r_{l}^2}\log{\left(b -
b_c\right) + \widetilde{C}(b)}$. We also numerically plot the images of shadows
and photon rings of the QBH in three different illumination models and compare
them with that of a Schwarzschild in each model. It is found that we could
distinguish the quantum black hole with a Schwarzschild black hole by the
shadow images in certain specific illumination model.
