We report on the results from a Chandra ACIS observation of the young , compact , supernova remnant N103B .
The unprecedented spatial resolution of Chandra reveals sub-arcsecond structure , both in the brightness and in spectral variations .
Underlying these small-scale variations is a surprisingly simple radial structure in the equivalent widths of the strong Si and S emission lines .
We investigate these radial variations through spatially resolved spectroscopy using a plane-parallel , non-equilibrium ionization model with multiple components .
The majority of the emission arises from components with a temperature of 1 keV : a fully ionized hydrogen component ; a high ionization timescale ( n _ { e } t > 10 ^ { 12 } s cm ^ { -3 } ) component containing Si , S , Ar , Ca , and Fe ; and a low ionization timescale ( n _ { e } t \sim 10 ^ { 11 } s cm ^ { -3 } ) O , Ne , and Mg component .
To reproduce the strong Fe K \alpha line , it is necessary to include additional Fe in a hot ( > 2 keV ) , low ionization ( n _ { e } t \sim 10 ^ { 10.8 } s cm ^ { -3 } ) component .
This hot Fe may be in the form of hot Fe bubbles , formed in the radioactive decay of clumps of ^ { 56 } Ni .
We find no radial variation in the ionization timescales or temperatures of the various components .
Rather , the Si and S equivalent widths increase at large radii because these lines , as well as those of Ar and Ca , are formed in a shell occupying the outer half of the remnant .
A shell of hot Fe is located interior to this , but there is a large region of overlap between these two shells .
In the inner 30 % of the remnant , there is a core of cooler , 1 keV Fe .
We find that the distribution of the ejecta and the yields of the intermediate mass species are consistent with model prediction for Type Ia events .