Planetary nebula Created 2026-10-05 Updated 2026-11-05
A planetary nebula is expelled stellar gas illuminated and ionized by a hot central remnant after an evolved star loses its outer envelope. It belongs to late stellar evolution, despite its historical name suggesting a planet. Ultraviolet photons from the exposed hot core cause photoionization; subsequent atomic processes produce prominent emission lines.[ref]
Planetary Nebula by European Space Agency. Definition and explanation of ionization of the expelled outer layers by the central star
The planetary-nebula spectral energy distribution can combine those lines with continua and thermal emission from dust. Spectroscopy therefore measures more than a colour: line ratios diagnose gas conditions, while Doppler shifts trace expansion. The Zanstra method connects nebular light to the central star's ionizing output. The central remnant subsequently follows white-dwarf cooling as the surrounding gas disperses.
Sirius Created 2026-10-18 Updated 2026-11-05
Sirius is a nearby binary star containing a luminous main-sequence star and a much fainter white dwarf. Their coexistence makes a useful lesson in stellar appearance: a hot object can be faint because its radiating area is small. The resolved Hubble Space Telescope image separates the compact companion from the bright primary's surrounding light.[ref]
The Dog Star, Sirius A, and its tiny companion by European Space Agency. Image description: Sirius A and its small, faint white-dwarf companion
The common orbit provides dynamical information, whereas spectral classification and luminosity constrain the two bodies' physical states. The white dwarf records prior stellar evolution; its current faintness does not mean it was always the less massive or less luminous member. Sirius therefore connects binary star measurements with white-dwarf cooling and the interpretation of the Hertzsprung-Russell diagram.
White-dwarf cooling 2026-11-05
White-dwarf cooling is the gradual loss of a white dwarf's stored thermal energy after sustained core fusion has ended. Dense degenerate electrons provide most of the pressure support, so luminosity can decline while the star remains mechanically supported.
Cooling depends on core heat capacity, envelope insulation, early neutrino losses and later crystallization processes. A population's luminosity distribution therefore contains age information only through a cooling model and its formation history. Crystallization can delay the decline through latent heat and compositional energy release; luminosity is not a simple universal linear clock.