convection zone

The region of the star in which this happens is the convection zone.

That is, most if not all of the star forms an extended convection zone.

He therefore replaced the model by including the effects of a thick convection zones on a star's interior.

This may be caused by the disappearance of a helium convection zone near the surface.

The heat travels from the radiative core to the star's surface through a convection zone.

"A field effect, maybe, from pressure waves originating in the solar convection zone.

Solar pressure waves are believed to be generated by the turbulence in the convection zone near the surface of the sun.

They dropped through the photosphere until they were well within the convection zone beneath the surface of the sun.

Recent studies of the Sun indicate its convection zone rotates at nearly the same rate at all depths.

A- or F-type stars have at most thin convection zones and thus produce little coronal activity.

Type-B stars do not have a corona and lack a convection zone in their outer atmosphere.

This profile extends on roughly radial lines through the solar convection zone to the interior.

Beneath the sun's photosphere lies the convection zone.

These form a visible component of magnetic flux tubes that are formed within a star's convection zone.

The photosphere floats atop the deep hydrogen convection zones of the stellar interior.

It is believed that this convection zone creates the magnetic activity that generates sun spots.

Stars with the mass of Alpha Pavonis are believed not to have a convection zone near their surface.

Another example of convective overshoot is at the base of the convection zone in the solar interior.

This is in contrast to the Sun, which has a radiation zone centered on the core with an overlying convection zone.

Therefore, the core region forms a convection zone that uniformly mixes the hydrogen fuel with the helium product.

This topologically complex field is most likely generated by a dynamo formed from the deep convection zone in the star's outer envelope.

Consequently, there is a high temperature gradient in the core region, which results in a convection zone for more efficient energy transport.

If this is not the case, however, then the plasma becomes unstable and convection will occur, forming a convection zone.

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.

The outer layers form a convection zone where the gas material transports energy primarily through physical displacement of the gas.