= Delayed iron enrichment
Massive stars produce prompt enrichment through <core-collapse supernovae>, whereas a <Type Ia supernova> follows binary stellar evolution and contributes substantial iron after a distribution of delays. A <stellar population> formed rapidly before much delayed enrichment can have a larger alpha-element to iron ratio than a <stellar population> formed over a prolonged interval. Relative abundance also depends on the <initial mass function>, <stellar yields>, and gas exchange; this is a chemical clock with model assumptions.
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