Fast radio bursts ( FRBs ) are millisecond bursts of radio radiation whose progenitors so far remain mysterious .
Nevertheless , the timescales and energetics of the events have lead to many theories associating FRBs with young neutron stars .
Motivated by this , I explore the interaction of FRBs with young supernova remnants ( SNRs ) , and I discuss the potential observational consequences and constraints of such a scenario .
As the SN ejecta plows into the interstellar medium ( ISM ) , a reverse shock is generated that passes back through the material and ionizes it .
This leads to a dispersion measure ( DM ) associated with the SNR as well as a time derivative for DM .
Times when DM is high are generally overshadowed by free-free absorption , which , depending on the mass of the ejecta and the density of the ISM , may be probed at frequencies of 400 { MHz } to 1.4 { GHz } on timescales of \sim 100 - 500 { yrs } after the SN .
Magnetic fields generated at the reverse shock may be high enough to explain Faraday rotation that has been measured for one FRB .
If FRBs are powered by the spin energy of a young NS ( rather than magnetic energy ) , the NS must have a magnetic field \lesssim 10 ^ { 11 } -10 ^ { 12 } { G } to ensure that it does not spin down too quickly while the SNR is still optically thick at radio frequencies .
In the future , once there are distance measurements to FRBs and their energetics are better understood , the spin of the NS can also be constrained .