Thermal time scale

In astrophysics, the thermal time scale is an estimate of the lifetime of a star once its fuel reserves at its center are used up or if they were to disappear. Along with the nuclear and dynamical time scales, it is used to estimate the length of time a particular star will remain in a certain phase of its life and its lifespan if hypothetical conditions are met. In reality, the lifespan of a star is greater than what is estimated by the thermal time scale because as one fuel becomes scarce, another will generally take its place--hydrogen burning gives way to helium burning, which is replaced by carbon burning.

Stellar astrophysics

The size of a star as well as its energy output generally determine a star's thermal lifetime because the measurement is independent of the type of fuel normally found at its center. Indeed, the thermal time scale assumes that there is no fuel at all inside the star and simply predicts the length of time it would take for the resulting change in outputted energy to reach the surface of the star and become visually apparent to an outside observer.

\tau_{th} = \frac{\mbox{total energy}}{\mbox{rate of energy loss}} = \frac{GM^2}{RL}

where G is the gravitational constant, M is the mass of the star, R is the radius of the star, and L is the star's luminosity. As an example, the Sun's thermal time scale is approximately 30 million years. [1]

References

  1. ^ Mitalas, R.; Sills, K.R. (December 1992). "On the photon diffusion time scale for the sun". Astrophysical Journal 401: 759-. Bibcode 1992ApJ...401..759M. doi:10.1086/172103.