Find the external structure of the sun!

Schematic diagram of the external structure of the sun is as follows:

The part above the photosphere of the sun is collectively called the solar atmosphere. Across the entire electromagnetic spectrum, from radio, visible light to gamma rays, we can observe that they are divided into five main parts: temperature polar region, chromosphere, transition region, corona and solar circle. The solar circle may be the thinnest outer edge of the solar atmosphere, and it extends beyond Pluto's orbit and at the junction with interstellar matter. This junction is called the solar sheath, where a shear shock front is formed. The temperature of chromosphere, transition zone and corona is higher than that of the sun surface. The reason has not been confirmed, but the evidence indicates that Alvin Bo may have carried enough energy to carry out coronal heating.

The sun is the central celestial body of the solar system, accounting for 99.86% of the total mass of the solar system. The eight planets, asteroids, meteors, comets, exoneptune objects and interstellar dust in the solar system all revolve around the sun, and the sun revolves around the center of the Milky Way.

The sun is a star located in the center of the solar system, and it is almost an ideal sphere where hot plasma and magnetic field are intertwined. From the chemical composition, about three-quarters of the mass of the sun is hydrogen, and the rest is almost helium, including oxygen, carbon, neon, iron and other heavy elements with mass less than 2%. Nuclear fusion is used to release light and heat into space.

Extended data:

The solar atmosphere above the troposphere is called the solar photosphere. The photosphere is an opaque thin layer of gas with a thickness of about 500 kilometers. It defines the very clear boundary of the sun, from which almost all visible light is emitted.

The colored ball is on top of the light ball. The thickness is about 2000 kilometers. The temperature distribution of the sun gradually decreases from the core to the photosphere, but it rises abnormally in chromosphere, reaching tens of thousands of degrees at the top of chromosphere. Because the total amount of visible light emitted by chromosphere is less than 1% of the photosphere, people usually can't see it.

Only when there is a total solar eclipse, a few seconds before the solar eclipse or a few seconds after the birth of light, the bright light emitted by the light ball is completely covered by the moon shadow for a short time, a narrow rose-red luminous aperture layer appears on the edge of the sun surface, which is the color ball. Usually, scientists can only observe the chromosphere of the sun through a monochromatic chromosphere telescope.

Corona is the outermost layer of the solar atmosphere, which is composed of high temperature and low density plasma. The brightness is weak, and the total brightness in white light is less than 1% of the brightness of the sun's circular surface, which is about equivalent to the brightness of the full moon. Therefore, it can only show its brilliance during the total solar eclipse, and it is usually observed with a special coronagraph. The temperature of the corona is as high as 1 million degrees, and its size and shape are related to solar activity. In the year of maximum solar activity, the corona is close to a circle. In quiet years, it is oval.

From ancient times to the present, the traditional way to observe the corona is to wait for a rare total solar eclipse-in the dark sky background, the bright spherical surface of the sun is covered by the moon, and a blue-white light zone appears around the sun, which is the outermost atmosphere of the sun that people expect to observe-the corona.

References:

Sun-Baidu encyclopedia