White Dwarfs Massive Stars Supernovae Star Formation Red Giants Binary Stars Planetary Nebulae Neutron Stars Black Holes Red Supergiants Dying Stars White Dwarf Stars Star Clusters Star Explosions Star Life Cycle Young Stars Binary Star Systems Protostars Star Types Variable Stars Supergiant Stars Star Composition Giant Stars Sun-like Stars Sun Supernova Pre-Planetary Nebulae Brown Dwarfs Nucleosynthesis Element Formation Star Observation Nuclear Fusion Supergiants Star Classification Metallicity Star Systems Main-Sequence Stars Star Death Population III Stars Planetary Science Metal-Poor Stars Binary Systems Life Cycle of Stars Black Hole Formation Wolf-Rayet Stars Cosmic Events Low Metallicity Stars Star Mergers Triple Star Systems Metal-free Stars Stellar Death Planetary Nebula Post-Main-Sequence Stars Young Stellar Objects Stellar Mergers Binary Neutron Stars Planetary Consumption Type Ia Supernovae Star Collapse Star Interactions Gravitational Perturbations Progenitor Stars Cataclysmic Variables Star Birthline Low-Mass Stars Open Clusters Primordial Stars Solar System Giant Branch Stars Star-Forming Regions Explosion End-of-Life Stars Dwarf Stars Heavy Elements Supernova Mechanisms Exoplanets Companion Objects Magnetars Star Explosion Planetary Systems Core-Collapse Supernovae Pulsars Second-Generation Stars Dimming Early Universe Ionization Supernova Outcomes Core Collapse Multi-Star Systems Main-Sequence Lifetimes Compact Star Systems Starquakes Failed Stars Star Lifecycle Companion Stars Circumstellar Discs Cepheid Variables Hydrogen Burning Stellar Explosions Planetary Formation
Its near-absence of heavy elements gives a clean test of how the first supernovae seeded later generations of stars.
