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Stellar population
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In 1944, Walter Baade categorized groups of stars within the Milky Way into stellar populations. In the abstract of the article by Baade, he recognizes that Jan Oort originally conceived this type of
Artist's conception of the spiral structure of the Milky Way showing Baade's general population categories. The blue regions in the spiral arms are co
Artist's conception of the spiral structure of the Milky Way showing Baade's general population categories. The blue regions in the spiral arms are composed of the younger population I stars, while the yellow stars in the central bulge are the older population II stars. In reality, many population I stars are also found mixed in with the older population II stars.
Population I star Rigel with reflection nebula IC 2118
Population I star Rigel with reflection nebula IC 2118
Artist's impression of a field of population III stars 100 million years after the Big Bang.
Artist's impression of a field of population III stars 100 million years after the Big Bang.
Possible glow of population III stars imaged by NASA's Spitzer Space Telescope
Possible glow of population III stars imaged by NASA's Spitzer Space Telescope
Pair-instability supernova
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A pair-instability supernova is a type of supernova predicted to occur when pair production — the production of free electrons and positrons in the collision between atomic nuclei and energetic gamma
Stellar population
…Many theoretical stellar models show that most high-mass population III stars rapidly exhausted their fuel and likely exploded in extremely energetic pair-instability supernovae. Those explosions would have thoroughly dispersed their material, ejecting metals into the interstellar medium (ISM), to be incorporated into the later…
When a star is very massive, the gamma rays produced in its core can become so energetic that some of their energy is drained away into production of
When a star is very massive, the gamma rays produced in its core can become so energetic that some of their energy is drained away into production of particle and antiparticle pairs. The resulting drop in radiation pressure causes the star to partially collapse under its own huge gravity. After this violent collapse, runaway thermonuclear reactions (not shown here) ensue and the star explodes.
G299 Remnants Super Nova Type 1a 20150218
G299 Remnants Super Nova Type 1a 20150218