"We find that these stars have very low iron content compared to the observed carbon-enhanced stars with billionths of the solar abundance of iron.
Their simulations also showed the carbonaceous grains seeding the fragmentation of the gas cloud produced, leading to formation of low-mass 'giga-metal-poor' stars that can survive to the present day and possibly be found in future observations. The study modeled for the first time faint supernovae of metal-free first stars, which yielded carbon-enhanced abundance patterns through the mixing and fallback of the ejected bits. "We can get results from indirect measurements to get the mass distribution of metal-free stars from the elemental abundances of metal-poor stars," said Gen Chiaki, a post-doctoral researcher in the Center for Relativistic Astrophysics, School of Physics, Georgia Tech.Ĭhiaki is the lead author of a study published in the September 2020 issue of the Monthly Notices of the Royal Astronomical Society. Their composition reflects the nucleosynthesis, or fusion, of heavier elements from the first stars. One type of these second stars is called a carbon-enhanced metal-poor star. They're unlikely to ever be observed, lost to the mists of time.Īs the metal-free first stars collapsed and exploded into supernovae, they forged heavier elements such as carbon that seeded the next generation of stars. The first stars probably only lived a few million years, a drop in the bucket of the age of the universe, at about 13.8 billion years.
The bigger the star, the faster they burn out. These gases cooled, collapsed, and ignited into stars up to 1,000 times more massive than our sun.
They're hypothesized to have formed about 100 million years after the Big Bang out of universal darkness from the primordial gases of hydrogen, helium, and trace light metals.
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