I have provided a brief review of the formation of the first stars and
their radiative, chemical, and mechanical feedback that affects
subsequent structure and galaxy formation. Over the past decade, many
groups have used numerical simulations to study these astrophysics
events in the first billion years of the universe. Currently, the
general consensus is that Population III stars are still very massive
with a characteristic mass of tens
M
with
an unknown fraction in
binaries. The prospect of Population III binaries is exciting, and
their impact on the universe prior to reionization, such as
pre-ionization from X-rays, will be addressed in future studies. To
summarize, the radiation from Population III expels most of the gas
from the host halos, creating gas-poor halos that cannot form stars
for 10-50 Myr. The SNe from the first stars enriches the first
galaxies to a nearly uniform ~ 10-3
Z, and
ultimately leads to the demise of this unique population of stars. The gas
depletion, IGM pre-heating, and chemical enrichment all have a lasting
impact on the formation of the first galaxies. Hopefully we can
utilize these imprints to disentangle Population III stellar
properties from the most distant galaxies in the universe.