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By definition, each population group shows the trend where lower metal content indicates higher age of stars. Hence, the first stars in the universe (very low metal content) were deemed population III, old stars (low metallicity) as population II, and recent stars (high metallicity) as population I. [6] The Sun is considered population I, a ...
HE 1327-2326, discovered in 2005 by Anna Frebel and collaborators, [2] was the star with the lowest known iron abundance until SMSS J031300.36−670839.3 was discovered. [5] The star is a member of Population II stars , with a solar-standardised iron to hydrogen index [Fe/H], or metallicity , of −5.4±0.2.
The first generation of stars, known as Population III stars, formed within a few hundred million years after the Big Bang. [58] These stars were the first source of visible light in the universe after recombination. Structures may have begun to emerge from around 150 million years, and early galaxies emerged from around 180 to 700 million years.
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Because it is a Population II star, some suggestions have been raised that second generation star formation may have begun very early on. [7] The oldest-known star (confirmed) – SMSS J031300.36−670839.3, forms. 300 million years: First large-scale astronomical objects, protogalaxies and quasars may have begun forming.
HE 1523-0901 is the designation given to a red giant star in the Milky Way galaxy approximately 9,900 light-years from Earth. It is thought to be a second generation, Population II, or metal-poor, star ([Fe/H] = −2.95). The star was found in the sample of bright metal-poor halo stars from the Hamburg/ESO Survey by Anna Frebel and
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This means that SDSS J0018−0939 most likely preserved the elemental abundance ratios produced by a first-generation very-massive star. [7] First generation stars are expected to self-regulate their growth by radiative feedback in the formation process, and to achieve masses typically tens of times that of the Sun. A fraction of stars might ...