Chandra serendipitously observed the eclipsing ( 80 ^ { \circ } < i < 84 ^ { \circ } ) intermediate polar , XY Arietis ( =H0253+193 ) , in two separate but continuous observations five weeks apart .
XY Ari was in a quiescent state during both observations .
We pursue the study of phase-resolved spectra for this system focusing on the Fe K lines .
From the combined and separate data sets , we readily detect emission lines of iron near 6.4 , 6.7 , and 6.9 keV at better than 99 % significance in contrast to previous results .
We confirm the orbit-phased sinusoidal absorption column behavior first observed with Ginga as well as a sinusoid-like behavior as a function of spin phase .
The presence of the 6.4 , 6.7 , and 6.9 keV lines requires different ionization states with \xi < 2 ( 6.4 keV ) and { \xi } \sim 3.5-4 ( 6.7 and 6.9 keV ) that must vary with phase .
We also detect emission lines at 3.25 , 4.8 , and 5.4 keV that are not instrumental in origin .
The 4.8 keV line may be identified as Ca XIX ( 4.832 keV ) and the 3.25 keV line may be Ar I K , but the 5.4 keV line has no obvious identification .