Linked from

The 11 pages that link to Convection zone, each with the reason it gives.

• Stellar structureCompared with: Its nearly adiabatic temperature gradient differs from the steep gradient in radiative regions.

• AsteroseismologyRelated: Convection excites many observable oscillations and affects their measured amplitudes.

• Solar luminosityBroader topic: Convection carries energy from the Sun’s interior toward its visible surface.

• Stellar activityRelated: Its turbulent motions help drive magnetic activity in stars with outer convection zones.

• Radiative zoneCompared with: Convection replaces radiative transport where the temperature gradient becomes sufficiently steep.

• Mass–luminosity relationRelated: Convection changes the internal temperature gradient and contributes to mass-dependent stellar structure.

• Stellar coreCompared with: Convection can replace radiation as the dominant transport process near or within some stellar cores.

• PhotosphereRelated: In the Sun, convection below the photosphere drives the visible granulation.

• Stellar opacityBroader topic: Opacity helps determine where radiative transport becomes unstable and convection begins.

• Hayashi trackRelated: Young low-mass stars on Hayashi tracks are largely or entirely convective.

• Chemically peculiar starRelated: Mixing can erase the element separations that diffusion would otherwise build.