  Modern cosmological simulations predict that the first generation of stars
formed with a mass scale around 100 solar masses about 300-400 million years
after the Big Bang. When the first stars reached the end of their lives, many
of them might have died as energetic supernovae that could have significantly
affected the early Universe via injecting large amounts of energy and metals
into the primordial intergalactic medium. In this paper, we review the current
models of the first supernovae by discussing on the relevant background
physics, computational methods, and the latest results.
