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We present an archival Chandra study of the O-rich supernova remnant (SNR) 1E0102.2-7219 in the Small Magellanic Cloud. Based on the deep $\sim$ 265 ksarchival Chandra data we performed a detailed spatially resolved spectralanalysis of 1E 0102.2-7219. Our aim is to reveal the spatial and chemicalstructures of this remnant in unprecedented details. Radial profiles of O, Neand Mg abundances based on our analysis of regional spectra extracted alongnine different azimuthal directions of 1E 0102.2-7219 suggest the contactdiscontinuity at $\sim$ 5-5.5 pc from the geometric center of the X-rayemission of the SNR. We find that the metal-rich ejecta gas extends furtheroutward in west and southwest than in other directions of the SNR. The averageO/Ne, O/Mg and Ne/Mg abundance ratios of the ejecta are in plausible agreementwith the nucleosynthesis products from the explosion of a $\sim 40 M_\odot$progenitor. We estimate an upper limit on the Sedov age of $\sim 3500$ yr andexplosion energy of $\sim 1.8\times10^{51}$ erg for 1E 0102.2-7219. We discussthe implications of our results on the geometrical structure of the remnant,its circumstellar medium and the nature of the progenitor star. Our results donot fit with a simple picture of the reverse-shocked emission from a sphericalshell-like ejecta gas with a uniformly-distributed metal abundance and apower-law density along the radius of the SNR.

A Detailed Archival CHANDRA Study of the Young Core-Collapse Supernova Remnant 1E 0102.2-7219 in the Small Magellanic Cloud