  Observations have revealed a significant dark matter deficit in the
ultra-diffuse galaxy NGC1052-DF2 (DF2). It is widely accepted that the
formation of this unique galaxy can be attributed to the tidal stripping of its
host galaxy, NGC1052. In this study, we simulate the evolution of a satellite
system containing globular clusters (GCs) within an accreting host halo in the
framework of self-interacting dark matter (SIDM). Our simulation results
suggest that the heightened tidal stripping resulting from DM self-interactions
can give rise to the transformation of a conventional dwarf galaxy into a dark
matter deficit galaxy resembling DF2. By comparing the simulation results with
identical initial conditions in both the standard cold dark matter (CDM) and
SIDM models, we find that the latter is more likely to replicate the properties
of DF2. Furthermore, we demonstrate that a DF2 analog can also be produced on
an orbit with a greater pericenter distance by increasing the strength of DM
self-interactions. This suggests that the issue of extreme orbital parameters
can be mitigated by implementing the SIDM model. The distributions of the GC
population derived in our SIDM simulation are consistent with the observed
characteristics of DF2. For comparison, we also explored the potential for
achieving GC distributions in the context of CDM.
