24Mg28Si

24Mg28Si refers to the nuclear reaction in which a magnesium‑24 nucleus (24Mg) fuses with a silicon‑28 nucleus (28Si). Both reactants are stable isotopes: magnesium‑24 has 12 protons and 12 neutrons, while silicon‑28 contains 14 protons and 14 neutrons. The combined system has a mass number of 52 and 26 protons, corresponding to titanium‑52 (52Ti) if the reaction proceeds via complete fusion. Because the end product is typically an excited nucleus, it can de‑excite by emitting gamma rays, neutrons, protons, or alpha particles, depending on the available energy and reaction channel.

In stellar environments, the 24Mg + 28Si fusion reaction is significant during advanced stages of massive star evolution, particularly in the oxygen and silicon burning phases. Temperatures above 1–2×10⁸ K and high densities enable thermonuclear reactions that build heavier nuclei. The reaction contributes to the synthesis of intermediate‑mass elements and provides a pathway for the production of isotopes such as 48Ti and 52Fe through subsequent beta decays. The reaction cross section peaks at energies around a few MeV in the center‑of‑mass frame and is sensitive to resonant states in the compound nucleus.

Laboratory experiments on the 24Mg + 28Si system employ heavy‑ion accelerators, with target foils of enriched 28Si and projectiles of 24Mg ions. Detection of emitted particles and gamma rays allows determination of resonance energies, widths, and branching ratios. These data are essential for refining nuclear reaction models used in astrophysical reaction network calculations.

The 24Mg28Si reaction exemplifies the complex interplay of nuclear structure and reaction dynamics that underpins stellar nucleosynthesis. Its study contributes both to the understanding of element formation in stars and to the development of accurate nuclear data for modeling explosive astrophysical events such as supernovae.