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Two main physical mechanisms are used to explain supernova explosions:thermonuclear explosion of a white dwarf(Type Ia) and core collapse of amassive star (Type II and Type Ib/Ic). Type Ia supernovae serve as distanceindicators that led to the discovery of the accelerating expansion of theUniverse. The exact nature of their progenitor systems however remain unclear.Radio emission from the interaction between the explosion shock front and itssurrounding CSM or ISM provides an important probe into the progenitor star'slast evolutionary stage. No radio emission has yet been detected from Type Iasupernovae by current telescopes. The SKA will hopefully detect radio emissionfrom Type Ia supernovae due to its much better sensitivity and resolution.There is a 'supernovae rate problem' for the core collapse supernovae becausethe optically dim ones are missed due to being intrinsically faint and/or dueto dust obscuration. A number of dust-enshrouded optically hidden supernovaeshould be discovered via SKA1-MID/survey, especially for those located in theinnermost regions of their host galaxies. Meanwhile, the detection ofintrinsically dim SNe will also benefit from SKA1. The detection rate willprovide unique information about the current star formation rate and theinitial mass function. A supernova explosion triggers a shock wave which expelsand heats the surrounding CSM and ISM, and forms a supernova remnant (SNR). Itis expected that more SNRs will be discovered by the SKA. This may decrease thediscrepancy between the expected and observed numbers of SNRs. Several SNRshave been confirmed to accelerate protons, the main component of cosmic rays,to very high energy by their shocks. This brings us hope of solving theGalactic cosmic ray origin's puzzle by combining the low frequency (SKA) andvery high frequency (Cherenkov Telescope Array: CTA) bands' observations ofSNRs.

Investigations of supernovae and supernova remnants in the era of SKA