You're close to the boundary of the radiative zone; the center of the Sun is another seven hundred thousand miles below you.

You're passing through the boundary layer between the radiative and connective zones, is all, Scholes said with studied calm.

Main sequence stars below about 0.3 solar masses are entirely convective, meaning they do not have a radiative zone.

Stars between 0.5 and 3 solar masses develop a radiative zone prior to reaching the main sequence.

This allows a radiative zone to develop around the star's core.

The radiative zone and the convective zone are separated by a transition layer, the tachocline.

The layer between the Sun's convective and radiative zone is called the tachocline.

In the classic solar model heat generated by nuclear fusion reactions at the star's center escapes through a radiative zone just outside the core.

The radiative zones of O-type main-sequence stars occur between the core and photosphere.

Stars with several times the mass of the Sun have a convection zone deep within the interior and a radiative zone in the outer layers.