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The ejecta kinematics of supernova remnants (SNRs) is one of crucial clues tounderstand the explosion mechanism of type Ia supernovae (SNe). In particular,the kinematic asymmetry of iron-peak elements provides the key to understandingphysical processes taking place in the core of the exploding white dwarfs (WDs)although it has been poorly understood by observations. In this paper, we showfor the first time the asymmetric expansion structure in the line-of-sightdirection of Fe ejecta in Kepler's SNR revealed by spectral and imaginganalysis using the Chandra archival data. We found that the K$\alpha$ linecentroid energy and line width is relatively lower ($<$ 6.4 keV) and narrower($\sim$80 eV) around the center of the remnant, which implies that the majorityof the Fe ejecta in the central region is red-shifted. At the outer regions, weidentify bright blue-shifted structures as it might have been ejected as highvelocity dense clumps. Taking into account the broad population of the Fecharge states, we estimate the red-shifted velocity of ~2,000 km/s and theblue-shifted velocity of ~3,000 km/s for each velocity structure. We alsopresent a possibility that a portion of the Fe ejecta near the center areinteracting with the dense circumstellar medium (CSM) on the near side of theremnant. As the origin of the asymmetric motion of the Fe ejecta, we suggestthree scenarios, (1) the asymmetric distribution of the CSM, (2) the "shadow"in Fe cast by the companion star, and (3) the asymmetric explosion.

Asymmetric Expansion of the Fe ejecta in Kepler's Supernova Remnant