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Context: Manganese is predominantly synthesised in Type Ia supernova (SN Ia)explosions. Owing to the entropy dependence of the Mn yield in explosivethermonuclear burning, SNe Ia involving near Chandrasekhar-mass white dwarfs(WDs) are predicted to produce Mn to Fe ratios significantly exceeding those ofSN Ia explosions involving sub-Chandrasekhar mass primary WDs. Of all currentsupernova explosion models, only SN Ia models involving near-Chandrasekhar massWDs produce [Mn/Fe] > 0.0. Aims: Using the specific yields for competing SN Iascenarios, we aim to constrain the relative fractions of explodingnear-Chandrasekhar mass to sub-Chandrasekhar mass primary WDs in the Galaxy.Methods: We extract the Mn yields from three-dimensional thermonuclearsupernova simulations referring to different initial setups and progenitorchannels. We then compute the chemical evolution of Mn in the Solarneighborhood, assuming SNe Ia are made up of different relative fractions ofthe considered explosion models. Results: We find that due to the entropydependence of freeze-out yields from nuclear statistical equilibrium, [Mn/Fe]strongly depends on the mass of the exploding WD, with near-Chandraskher massWDs producing substantially higher [Mn/Fe] than sub-Chandrasekhar mass WDs. Ofall nucleosynthetic sources potentially influencing the chemical evolution ofMn, only explosion models involving the thermonuclear incineration ofnear-Chandrasekhar mass WDs predict solar or super-solar [Mn/Fe]. Consequently,we find in our chemical evolution calculations that the observed [Mn/Fe] in theSolar neighborhood at [Fe/H] > 0.0 cannot be reproduced withoutnear-Chandrasekhar mass SN Ia primaries. Assuming that 50 per cent of all SNeIa stem from explosive thermonuclear burning in near-Chandrasekhar mass WDsresults in a good match to data.

Solar abundance of manganese: a case for the existence of near Chandrasekhar-mass Type Ia supernova progenitors