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We present a second epoch of {\it Chandra} observations of the Type Ia LMCSNR 0509-68.7 (N103B) obtained in 2017. When combined with the earlierobservations from 1999, we have a 17.4-year baseline with which we can searchfor evidence of the remnant's expansion. Although the lack of strong pointsource detections makes absolute image alignment at the necessary accuracyimpossible, we can measure the change in the diameter and the area of theremnant, and find that it has expanded by an average velocity of 4170 (2860,5450) km s$^{-1}$. This supports the picture of this being a young remnant;this expansion velocity corresponds to an undecelerated age of 850 yr, makingthe real age somewhat younger, consistent with results from light echo studies.Previous infrared observations have revealed high densities in the western halfof the remnant, likely from circumstellar material, so it is likely that thereal expansion velocity is lower on that side of the remnant and higher on theeastern side. A similar scenario is seen in Kepler's SNR. N103B joins the rareclass of Magellanic Cloud SNRs with measured proper motions.

The Expansion of the Young Supernova Remnant 0509-68.7 (N103B)