  The accretion disks of supermassive black holes (SMBHs) harboring in active
galactic nuclei (AGN) are considered to be an ideal site for producing
different types of gamma-ray bursts (GRBs). The detectability of these GRB
phenomena hidden in AGN disks is highly dependent on the dynamical evolution of
the GRB relativistic jets. By investigating the reverse and forward shock
dynamics due to the interaction between the jets and AGN disk material, we find
that the relativistic jets can successfully break out from the disks only for a
sufficiently high luminosity and a long enough duration. In comparison,
relatively normal GRB jets are inclined to be choked in the disks, unless the
GRBs occur near an SMBH with relatively low mass (e.g., $\sim 10^6M_{\odot}$).
For the choked jets, unlike normal GRB prompt and afterglow emission, we can
only expect to detect emission from the forward shock when the shock is very
close to the edge of the disks, i.e., the shock breakout emission and
subsequent cooling of the shock.
