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Type Ia supernova (SNIa) explosions synthesize a few tenths to several tenthsof a solar mass, whose composition is the result of incomplete silicon burningthat reaches peak temperatures of 4 GK to 5 GK. The elemental abundances aresensitive to the physical conditions in the explosion, making their measurementa promising clue to uncovering the properties of the progenitor star and of theexplosion itself. Using a parameterized description of the thermodynamichistory of matter undergoing incomplete silicon burning, we computed the finalcomposition for a range of parameters wide enough to encompass current modelsof SNIa. Then, we searched for combinations of elemental abundances that tracethe parameters values and are potentially measurable. For this purpose, wedivide the present study into two epochs of SNIa, namely the optical epoch,from a few weeks to several months after the explosion, and the X-ray epoch,which refers to the time period in which the supernova remnant is young,starting one or two hundred years age and ending a thousand years after theevent. During the optical epoch, the only SNIa property that can be extractedfrom the detection of incomplete silicon burning elements is the neutron excessof the progenitor white dwarf at thermal runaway, which can be determinedthrough measuring the ratio of the abundance of manganese to that of titanium,chromium, or vanadium. Conversely, in the X-ray epoch, any abundance ratiobuilt using a couple of elements from titanium, vanadium, chromium, ormanganese may constrain the initial neutron excess. Furthermore, measuring theratio of the abundances of vanadium to manganese in the X-ray might shed lighton the timescale of the thermonuclear explosion.

Insights into thermonuclear supernovae from the incomplete silicon burning process