  Supernova remnants (SNRs) are important objects in investigating the links
among supernova (SN) explosion mechanism(s), progenitor stars, and cosmic-ray
acceleration. Non-thermal emission from SNRs is an effective and promising tool
for probing their surrounding circumstellar media (CSM) and, in turn, the
stellar evolution and mass-loss mechanism(s) of massive stars. In this work, we
calculate the time evolution of broadband non-thermal emissions from Type Ib/c
SNRs whose CSM structures are derived from the mass-loss history of their
progenitors. Our results predict that Type Ib/c SNRs make a transition of
brightness in radio and $\gamma$-ray bands from an undetectable dark for a
certain period to a re-brightening phase. This transition originates from their
inhomogeneous CSM structures in which the SNRs are embedded within a
low-density wind cavity surrounded by a high-density wind shell and the ambient
interstellar medium (ISM). The "resurrection" in non-thermal luminosity happens
at an age of ~1,000 yrs old for a Wolf-Rayet star progenitor evolved within a
typical ISM density. Combining with the results of Type II SNR evolution
recently reported by Yasuda et al. (2021), this result sheds light on a
comprehensive understanding of non-thermal emissions from SNRs with different
SN progenitor types and ages, which is made possible for the first time by the
incorporation of realistic mass-loss histories of the progenitors.

High Energy Astrophysical Phenomena