---
title: "Where a dead star keeps its heat"
description: "Separate degenerate support from thermal energy. Count ions, derive a first cooling time and distinguish core temperature from the photosphere."
canonical_url: "https://sandboxphysics.com/stories/white-dwarf-cooling/degenerate-support-and-stored-heat/"
language: "en"
page_type: "story"
alternate_languages:
  zh-CN: "https://sandboxphysics.com/zh/stories/white-dwarf-cooling/degenerate-support-and-stored-heat/"
last_modified: "2026-11-03"
---

[The heat and clocks of white dwarfs](https://sandboxphysics.com/stories/white-dwarf-cooling/)

L1 · White dwarf cooling and crystallization

# Where a dead star keeps its heat

Sandbox Physics · 2026-11-03

A cooling white dwarf stays supported mainly by degenerate electrons while losing thermal energy stored in its particles. To estimate a cooling time, count that thermal reservoir and the rate at which energy leaves. The pressure supporting the star is not itself the luminosity.

## Before you begin

Read Why white dwarfs cool so slowly. You need conservation of energy, density, scientific notation and the meaning of a derivative as a rate of change.

## Choose an energy reservoir before assigning a time

Take a fixed amount of dense carbon matter. Let its volume and composition remain unchanged, and give it a uniform temperature. These restrictions remove contraction work and composition changes from the first calculation. We also set nuclear heating and neutrino losses to zero. The remaining problem is to balance the decline of thermal energy against the light leaving the object.

Write the thermal energy as $U(T)$ in ergs, temperature $T$ in kelvin and outward luminosity $L$ in ergs per second. One erg is one ten-millionth of a joule. Define the heat capacity $C=dU/dT$: it is the extra energy required to increase this fixed object’s temperature by one kelvin.

A positive luminosity removes energy. Consequently temperature falls when the heat capacity is positive. That sign matters: a solution in which an isolated object warms while radiating would require an additional energy source. When heat capacity and luminosity are approximately constant over a stated interval, the time follows directly from the energy lost.

$$
\frac{dU}{dt}=C\frac{dT}{dt}=-L,\qquad\Delta t=\frac{C(T_i-T_f)}{L}
$$

The initial temperature $T_i$ exceeds the final temperature $T_f$. The second expression assumes constant heat capacity and luminosity during the interval.

Sources: [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583) · [Bauer 2023, Carbon-Oxygen Phase Separation in MESA White Dwarf Models, arXiv2303.10110v2, Eq1–8 and §§2–5](https://arxiv.org/abs/2303.10110v2)

## The electrons that support the star are strongly degenerate

Electron degeneracy means the low-energy quantum states are densely occupied. Compression forces electrons into states with higher momentum, producing pressure even when the thermal temperature is low. A large supporting pressure can therefore survive as the star cools.

Heating such electrons mainly changes the occupation of states near the boundary between filled and empty states. It does not give every electron the full thermal freedom of a dilute gas. Their heat capacity can be small compared with what a classical gas estimate would suggest, and falls with temperature in the strongly degenerate limit.

The ions carry a different reservoir. Their motion and interactions store thermal energy, while the electrons supply much of the pressure and transport heat efficiently. Later in cooling, the ionic heat capacity drops as the solid’s vibrations become quantum mechanical; the remaining electron term can become comparatively important. The temperature and density determine which component holds more thermal energy.

Sources: [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583) · [Bauer 2023, Carbon-Oxygen Phase Separation in MESA White Dwarf Models, arXiv2303.10110v2, Eq1–8 and §§2–5](https://arxiv.org/abs/2303.10110v2) · [MIST white dwarf models, arXiv2509.21717v1, cooling clocks, surface boundary and model comparisons](https://arxiv.org/abs/2509.21717v1)

## Count ions, then specify their heat capacity

Let the matter have total mass $M$ and consist of nuclei with mass number $A$. With atomic mass unit $m_u$ in grams, the ion count is approximately mass divided by the mass of one nucleus. For pure carbon, the mass number is twelve.

Heat capacity needs another physical assumption. A dilute monatomic gas has three kinetic degrees of freedom and a heat capacity of one and a half times the ion count times Boltzmann’s constant. In a classical harmonic solid, kinetic and potential energy both contribute, giving three times that product at sufficiently high temperature. These two results describe different material states.

The controlled core model adopts the latter constant value for its liquid sensible branch and uses a Debye solid below melting. That liquid choice is an explicit approximation, not a derivation of the exact heat capacity of a strongly interacting plasma. A detailed stellar EOS calculates the thermal response from a more complete description of the material.

$$
N_i=\frac{M}{A m_u},\qquad C_{\rm gas}=\frac32N_i k_B,\qquad C_{\rm classical\ solid}=3N_i k_B
$$

The ion count is $N_i$; Boltzmann’s constant is $k_B=1.380649\times10^{-16}\,\mathrm{erg\,K^{-1}}$. The solid expression applies in its high-temperature harmonic limit; another material state needs its corresponding heat capacity.

Sources: [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583) · [Bauer 2023, Carbon-Oxygen Phase Separation in MESA White Dwarf Models, arXiv2303.10110v2, Eq1–8 and §§2–5](https://arxiv.org/abs/2303.10110v2) · [MESA 22.11.1 fixed const\_def.f90, matching original source units](https://github.com/MESAHub/mesa/blob/22.11.1/const/public/const_def.f90)

## A first cooling-time calculation

Consider a hypothetical pure-carbon reservoir with mass $0.6M_\odot$. For this exercise specify $C=3N_i k_B$ and a constant luminosity $10^{-3}L_\odot$. Let it cool through one million kelvin without a phase transition. These are the problem’s assumptions; we are not assigning an observed white dwarf that age.

Using the declared MESA units, $M_\odot=1.988409870698051\times10^{33}\,\mathrm g$, $L_\odot=3.828\times10^{33}\,\mathrm{erg\,s^{-1}}$ and $m_u=1/(6.02214076\times10^{23})\,\mathrm g$, the reservoir contains about $5.99\times10^{55}$ ions. Its specified heat capacity is $2.48\times10^{40}\,\mathrm{erg\,K^{-1}}$.

Multiply that heat capacity by the temperature drop to get $2.48\times10^{46}\,\mathrm{erg}$. Divide by $3.828\times10^{30}\,\mathrm{erg\,s^{-1}}$ and then by the seconds in a year. The result is about $2.05\times10^8\,\mathrm{yr}$, or 205 million years. The units cancel to time; the result is positive because the final temperature is lower.

Doubling the specified luminosity halves this interval. Doubling the mass would double the specified heat reservoir, but it would not necessarily double the age of a real white dwarf: a different stellar mass also changes density, radius and luminosity. The simple calculation teaches how energy becomes a time only after the model’s other quantities are fixed.

$$
\Delta t=\frac{(2.48\times10^{40}\,\mathrm{erg\,K^{-1}})(10^6\,\mathrm K)}{3.828\times10^{30}\,\mathrm{erg\,s^{-1}}}\simeq2.05\times10^8\,\mathrm{yr}
$$

This rounded worked value is independently computed by compute\_textbook\_examples.py; it uses a fixed reservoir and constant luminosity, not a native stellar age.

Sources: [MESA 22.11.1 fixed const\_def.f90, matching original source units](https://github.com/MESAHub/mesa/blob/22.11.1/const/public/const_def.f90) · [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583)

## Connect the core to the light at the surface

A white dwarf is not an exposed lump with a chosen constant luminosity. Heat crosses the outer layers before escaping. A surface atmosphere supplies a relation among effective temperature, gravity and outgoing radiation, while the deeper envelope connects that surface to the hot interior.

The effective surface temperature $T_{\rm eff}$ is defined through the total outgoing flux. For radius $R$ and Stefan–Boltzmann constant $\sigma$, the relation below defines the luminosity. It does not say that the observed spectrum is a perfect blackbody, nor that the core has the same temperature.

The next chapter derives a controlled radiative-envelope relation and then adds freezing. A full white-dwarf calculation uses a stellar structure and EOS together with appropriate atmospheric boundary conditions. The long controlled-model clocks in the figure are left visible because a consistent energy calculation alone does not calibrate an actual stellar age.

$$
L=4\pi R^2\sigma T_{\rm eff}^4
$$

Effective temperature describes the surface energy flux. The approximately uniform core temperature $T_c$ belongs to a different physical location.

![Controlled pure-carbon solid fractions against independent model time and imposed core temperature for four frozen density geometries](https://sandboxphysics.com/stories/white-dwarf-cooling/materials/controlled-core-phase.png)

Controlled pure-carbon calculations on four fixed source density geometries. Left: uncalibrated elapsed model time; the very long times are not stellar-age estimates. Right: solid fraction against imposed core temperature. The vertical axis is the solid fraction of the selected core mass.

Sources: [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583) · [MIST white dwarf models, arXiv2509.21717v1, cooling clocks, surface boundary and model comparisons](https://arxiv.org/abs/2509.21717v1) · [Bauer 2023, fixed MESA inputs and starting models, Zenodo 7846751, CC BY 4.0](https://doi.org/10.5281/zenodo.7846751)

## Work through the question

If degenerate pressure supports the star, why does a cooling calculation still need an ionic heat capacity?

Pressure describes the mechanical response to compression. Heat capacity describes the change of energy with temperature. The ions can store substantial thermal energy even when electrons provide most of the supporting pressure.

Keep the exercise’s reservoir fixed but use luminosity $2\times10^{-3}L_\odot$. What happens to the cooling interval?

The luminosity doubles while the required energy loss is unchanged, so the time halves to about $1.03\times10^8\,\mathrm{yr}$. The heat capacity and luminosity remain fixed throughout this exercise.

A student replaces core temperature with measured surface effective temperature in the reservoir calculation. What information is missing?

The atmosphere and envelope relation is missing. Surface radiation and internal thermal energy refer to different locations; one must connect them with a transport/boundary model before inferring a time.

### [Probe liquid and solid material](https://sandboxphysics.com/labs/white-dwarf-crystallization/)

1. Pause the default partially frozen core and move only the radial probe. Compare phase and density at two radii.
2. Check that the imposed core temperature remains uniform when you move the probe; the colours describe phase and lighting.
3. Choose the liquid-reservoir demo, then describe which part of the energy balance is supplying the emitted light.

## Primary sources

1. [Mestel 1952, On the theory of white dwarf stars, MNRAS112583–597, thermal §§2–4](https://doi.org/10.1093/mnras/112.6.583)
2. [Bauer 2023, Carbon-Oxygen Phase Separation in MESA White Dwarf Models, arXiv2303.10110v2, Eq1–8 and §§2–5](https://arxiv.org/abs/2303.10110v2)
3. [Bauer 2023, fixed MESA inputs and starting models, Zenodo 7846751, CC BY 4.0](https://doi.org/10.5281/zenodo.7846751)
4. [MIST white dwarf models, arXiv2509.21717v1, cooling clocks, surface boundary and model comparisons](https://arxiv.org/abs/2509.21717v1)
5. [MESA 22.11.1 fixed const\_def.f90, matching original source units](https://github.com/MESAHub/mesa/blob/22.11.1/const/public/const_def.f90)

[Previous: Why white dwarfs cool so slowly](https://sandboxphysics.com/stories/white-dwarf-cooling/why-white-dwarfs-cool-slowly/) [Next: How crystallization slows white dwarf cooling](https://sandboxphysics.com/stories/white-dwarf-cooling/latent-heat-and-white-dwarf-cooling/)