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We show that the X-ray line flux of the Mn Kalpha line at 5.9 keV from thedecay of 55Fe is a promising diagnostic to distinguish between Type Iasupernova (SN Ia) explosion models. Using radiation transport calculations, wecompute the line flux for two 3D explosion models: a near-Chandrasekhar massdelayed detonation and a violent merger of two white dwarfs. Both models arebased on solar metallicity zero-age main sequence progenitors. Due to explosivenuclear burning at higher density, the delayed-detonation model synthesises 3.5times more radioactive 55Fe than the merger model. As a result, we find thatthe peak Mn Kalpha line flux of the delayed-detonation model exceeds that ofthe merger model by a factor of 4.5. Since in both models the 5.9 keV X-rayflux peaks five to six years after the explosion, a single measurement of theX-ray line emission at this time can place a constraint on the explosionphysics that is complementary to those derived from earlier phase opticalspectra or light curves. We perform detector simulations of current and futureX-ray telescopes to investigate the possibilities of detecting the X-ray lineat 5.9 keV. For the delayed-detonation scenario, a line detection is feasiblewith Chandra up to 3 Mpc for an exposure time of 10^6 s. We find that it shouldbe possible with currently existing X-ray instruments (with exposure times5x10^5 s) to detect both of our models at sufficiently high S/N to distinguishbetween them for hypothetical events within the Local Group. The prospects fordetection will be better with future missions. For example, the proposedAthena/X-IFU instrument could detect our delayed-detonation model out to adistance of 5 Mpc. This would make it possible to study future events occurringduring its operational life at distances comparable to those of the recentsupernovae SN 2011fe (6.4 Mpc) and SN 2014J (3.5 Mpc).

5.9 keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models