What is the radiation and convection zone in the Solar System?

Have you ever heard of concepts like radiation or convection? What are these concepts in the Solar System?

The sun - the star in the solar system and the source of energy and natural light for the Earth. But few know exactly what constitutes the Sun. One of the concepts you often hear is radiation and convection.

Radiation zone

The radiation zone is the region from 0.25 to about 0.7 in the Sun's radius, the Sun's material is hot enough and dense enough to heat the heat from the core out. There is no thermal convection in this area; although the materials cool when the altitude rises (from 7,000,000 ° C to about 2,000,000 ° C) this temperature gradient is smaller than the adiabatic lapse rate and therefore cannot causing convection. Heat is transmitted by radiation - the ion of hydrogen and helium emits photons, which only move a short distance before being reabsorbed by other ions. Actual photons pop up many times through this solid material to the point that a single photon takes about a million years to reach the surface layer, and thus, the energy moves out very slowly. Density decreases hundreds of times (from 20 g / cm³ down to only 0.2 g / cm³) from the bottom to the top of the radiation zone.

The radiation zone is the region from 0.25 to about 0.7 in the radius of the Sun.

Transition zone (tacholine)

Between the radiation and convection regions is a transition layer called tachocline. This is the region where there is a sharp shift between the rotational rotation of the radiation zone and the differential movement of the convection region leading to a strong slip — a condition where each other's horizontal layers slid over each other. Fluid-like forms of movement in the convection region above, gradually disappear from the top of this layer to its bottom, consistent with the quiet characteristics of the radiation zone on the bottom. Currently, there is a theory that a source of electricity from inside this layer produces the sun's magnetic field.

Convection area

In the outer layer of the Sun, from its surface to approximately 200,000 km (or 70% of the Sun's radius), the solar plasma is not dense enough or hot enough to transfer thermal energy from inside to out by radiation. Therefore, heat convection takes place when heat columns carry hot material to the sun's surface (light book). When the material cools at the surface, it goes down to the bottom of the convection area to receive more heat from the top of the radiation zone.

Heat columns in the convection zone create a trace on the Sun, in the form of solar granulation and super beads. The convective turbulence of this outer part of the interior of the Sun formed an emerging "small-scale" generator that produced polar and north magnetic fields across the entire Sun's surface.

The convection in the Solar System is considered the outer layer in the area inside the Sun. The temperature in this area is very cool, suitable for heavy mass ions such as carbon, nitrogen, oxygen, calcium, and iron in the electron state. These electrons are blocked and capable of absorbing more heat, thereby creating a process of boiling or plasma transformation.