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We investigate two multi-shell galactic supernova remnants (SNRs), Kes79 andG352.7-0.1, to understand the causes of such morphology. The research wascarried out based on new and reprocessed archival VLA observations andXMM-Newton archival data. The surrounding was investigated based on dataextracted from the HI Canadian Galactic Plane Survey, the 13^CO Galactic RingSurvey and the HI Southern Galactic Plane Survey. The present study revealedthat the overall morphology of both SNRs is the result of the mass-loss historyof their respective progenitor stars. Kes79 would be the product of thegravitational collapse of a massive O9 star evolving near a molecular cloud andwithin the precursor's wind-driven bubble, while G352.7-0.1 would be the resultof interactions of the SNR with an asymmetric wind from the progenitor togetherwith projection effects. No radio point source or pulsar wind nebula was foundassociated with the X-ray pulsar CXOU J185238.6+004020 in Kes79. The X-raystudy of G352.7-0.1, on its hand, revealed that most of the thermal X-rayradiation completely fills in the interior of the remnant and originates inheated ejecta. Characteristic parameters, like radio flux, radio spectralindex, age, distance, shock velocity, initial energy and luminosity, wereestimated for both SNRs.

Radio and X-ray study of two multi-shell Supernova Remnants: Kes79 and G352.7-0.1