Structure of the Sun

plasma "atmosphere" of the Sun

thumb|alt=A miasma of plasma|Sun's surface in false color|228x228px The photosphere is a star's outer shell from which light is radiated. It extends into a star's surface until the plasma becomes opaque, equivalent to an optical depth of approximately , or equivalently, a depth from which 50% of light will escape without being scattered.

The heliosphere is the magnetosphere, astrosphere, and outermost atmospheric layer of the Sun. It takes the shape of a vast, tailed bubble-like region of space. In plasma physics terms, it is the cavity formed by the Sun in the surrounding interstellar medium. The "bubble" of the heliosphere is continuously "inflated" by plasma originating from the Sun, known as the solar wind. Outside the heliosphere, this solar plasma gives way to the interstellar plasma permeating the Milky Way. As part of the interplanetary magnetic field, the heliosphere shields the Solar System from significant amounts o

thumb|The chromosphere emits predominantly deep red light of the Hα spectral line.

central region of the Sun

outer region of the volume of a star

(of a star) layer which is unstable to convection. Energy is primarily or partially transported by convection in such a region

radiative layer of stars

Section of Sun's atmosphere

300px|thumb|Internal rotation in the Sun, showing differential rotation in the outer convective region (as a function of latitude) and almost uniform rotation in the central radiative region. The transition between these regions is called the tachocline. To convert the y-axis to period, use 1 / 500 nanoHz = 23.15 days.

model of the Sun’s current state, evolution and interior

surface which separates the heliosphere into positively and negatively charged components

boundary between solar corona and wind