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The supernova remnant (SNR) 30 Dor B is associated with the \ion{H}{2} regionionized by the OB association LH99. The complex interstellar environment hasmade it difficult to study the physical structure of this SNR. We have usedHubble Space Telescope H$\alpha$ images to identify SNR shocks and deep ChandraX-ray observations to detect faint diffuse emission. We find that 30 Dor Bhosts three zones with very different X-ray surface brightnesses and nebularkinematics that are characteristic of SNRs in different interstellarenvironments and/or evolutionary stages. The ASKAP 888 MHz map of 30 Dor Bshows counterparts to all X-ray emission features except the faint halo. TheASKAP 888 MHz and 1420 MHz observations are used to produce a spectral indexmap, but its interpretation is complicated by the background thermal emissionand the pulsar PSR J0537$-$6910's flat spectral index. The stellar populationin the vicinity of 30 Dor B indicates a continuous star formation in the past8--10 Myr. The observed very massive stars in LH99 cannot be coeval with theprogenitor of 30 Dor B's pulsar. Adopting the pulsar's spin-down timescale,5000 yr, as the age of the SNR, the X-ray shell would be expanding at$\sim$4000 km\,s$^{-1}$ and the post-shock temperature would be 1--2 orders ofmagnitude higher than that indicated by the X-ray spectra. Thus, the brightcentral region of 30 Dor B and the X-ray shell requires two separate SN events,and the faint diffuse X-ray halo perhaps other older SN events.

New Insights on 30 Dor B Revealed by High-Quality Multi-wavelength Observations