White Dwarfs Massive Stars Supernovae Star Formation Red Giants Binary Stars Planetary Nebulae Neutron Stars Red Supergiants Black Holes White Dwarf Stars Star Clusters Dying Stars Binary Star Systems Star Explosions Star Life Cycle Young Stars Supergiant Stars Star Types Protostars Variable Stars Planetary Science Black Hole Formation Sun Binary Systems Life Cycle of Stars Star Composition Main-Sequence Stars Chemical Composition Sun-like Stars Metal-Poor Stars Giant Stars Supernova Pre-Planetary Nebulae Star Death Wolf-Rayet Stars Population III Stars Brown Dwarfs Nuclear Fusion Nucleosynthesis Star Observation Supergiants Star Classification Metallicity Ancient Stars Star Systems Stellar Ages Element Formation 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 Thermonuclear Explosions
The GMOS image links a long‑period binary’s winds to the nebula’s lumpy shells while recording light that left the object about 1,500 years ago.
