White dwarfs are the dense, cooling remnants of low‑ and intermediate‑mass stars. After nuclear burning ceases, they radiate away their residual thermal energy, gradually fading over billions of years. The rate at which a white dwarf cools depends primarily on its core composition, mass, and surface temperature.
The cooling process can be approximated by a power‑law relation between the effective temperature (Teff) and the elapsed cooling time (tcool). More massive white dwarfs have higher central densities, which slows heat transport and lengthens the cooling age for a given temperature.
This widget lets you estimate the cooling age of a white dwarf from its observed effective temperature and mass. By entering realistic values, you can explore how subtle changes in temperature or mass translate into gigayear‑scale age differences, a key tool for stellar population studies and Galactic archaeology.
How does the mass of a white dwarf affect its cooling time?
What is the relationship between a white dwarf's effective temperature and its cooling time?
Can you explain the role of core composition in white dwarf cooling?
How long does it typically take for a white dwarf to cool down completely?
What factors determine the cooling rate of a white dwarf?
Results are for informational purposes only and do not constitute professional advice.