Supernovae Novae Nova White Dwarfs Black Holes Stellar Evolution Binary Stars Supernova Star Formation Red Supergiants Variable Stars Planetary Systems Nebulae Planetary Nebulae Nova Events Massive Stars Binary Star System Novas Binary Systems Star Characteristics Binary Star Systems White Dwarf Stars Stellar Flares Star Disappearance Supergiants Nova Explosions Planetary Ingestion Explosions Recurrent Nova Red Dwarf Stars Flares Betelgeuse Star Interactions Coronal Mass Ejections Red Giants Red Giant Stars Stellar Winds Supernova Remnants Red Dwarfs Companion Stars Total Collapse Theory Observations Massive Star Collapse Disappearing Stars Observational Data Analysis Radio Emissions Thermonuclear Explosion Observing Celestial Events Convection Dust Clouds Energy Signatures Thermonuclear Explosions Celestial Events Observation Protostellar Outflows Accretion Discs Recurrent Novae Fast-Moving Stars Solar Flares Star Observations Accretion Disks Superflares Magnetars Solar Activity Blue Stragglers Fast-moving Stars Supernova Types Dwarf Stars Light Variations Ultraviolet Radiation Neutron Stars Nova Outburst White Dwarf Star Red Giant Star Nova Eruption Twin Stars Planetary Consumption Stellar Radio Emissions Planet-Eating Stars Blue Supergiant Stars Planet Ingestion Co-Natal Stars Planetary Devouring Type 1a Supernovae Stardust Presolar Grains Stellar Collisions Star Evolution Sun Star Collapse White Dwarf Star Life Cycle Stellar Cannibalism Gas Ejection Star-Planet Interactions Light Pulses Supermassive Black Holes Stellar Dimming Cataclysmic Variable Stars Exploding Stars
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The new NIRCam and MIRI observations let astronomers trace compact dust clumps, ionized-gas bubbles, and molecular signatures that explain how the central white dwarf sculpts the nebula.
