What are the different parts of the sun?

Answer 1

They are the Corona, the Visible Surface, the Solar and the Chromosphere. The sun is a huge hot ball of gases which are mostly hydrogen and helium. It has an innermost part, the core, in which light and heat energy are produced. The temperature in the core is about 15 million debgrees Celsius. The energy produced in the core travels to the surface in two ways. First, it travels in the form of radiant energy through the radiation zone. This zone has a temperature of 2.5 million degrees Celsius. From this zone. the energy travels by convection through the convection zone. Here, the gases undergo violent motions and carry most of the sun's energy to the surface of the sun. The photosphere, which is over 500 kilometers thick, is the apparent yellow surface of the sun. However, the sun is purely gaseous, so the photosphere is just the visible area of the sun's atmosphere. The temperature here is about 5500 degrees Celsius. Light is given off from the photosphere. The photosphere contains millions of granules. These are small patches of gases that look bright. A granule lasts for only a few minutes and then fades away. Other graanules take the places of those which have faded. The combined motion of all the granules makes the photosphere appear to be boiling. Extending about ten thousand kilometers from the photosphere is the chromosphere.

The chromosphere looks red because of glowing hydrogen gas. The top of the chromosphere contains spicules. These spicules are gas columns believed to be continuations of the violent motions of granules in the photosphere. Spicules can shoot about 16 000 kilometers into the corona. The outermost portion of the sun's atmosphere is the corona. It is estimated to have a height of more than a million kilometers. The corona is visible only when there is a total eclipse of the sun. When the sun's disk is darkened by the moon's shadow, the corona is seen as a faint light. At the corona's temperature of 1 million degrees Celsius, the particles of gas begin to escape the sun's gravity and flow outward into space. This flow of gas particles is called the solar wind. At a speed of 500 km/s, the solar wind takes a few days to reach Earth. Radiation, on the other hand, travels from the photosphere at the speed of light (3.0 x 10 to the fifth power km/s) and reaches Earth in eight minutes. The words with BOLD are the sun's parts namely: * core * photosphere * chromosphere * corona

Answer 2

The sun's layers

-the core: the thermonuclear reactions in this layer produce the Sun's light and energy

-the radiative zone: this layer's gases are as dense as water. Energy from the core flows outward through this layer towards the Sun's surface.

-the convection zone: in this layer, gases churn with violent motions to carry energy to the Sun's surface.

-the photosphere: this layer gives off the heat and light energy of the Sun. Sunspots, or cooler areas that can be seen from Earth, radiate here.

-the chromosphere: streams of gases, called spicules,shoot up from this layer of the Sun's light and heat.

-the corona: in this upper layer of the Sun's atmosphere, gases expand away from the Sun to create solar wind.

Answer 3

the 9 parts of the sun are: 1. Core

2. Radiative zone

3. Convective zone

4. Photosphere

5. Chromosphere

6. Corona

7. Sunspot

8. Granules

9. Prominence

Answer 4

Full solar radiation is determined by the light produced by them on the surface of the Earth - about 100 thousand lux, when the sun is at its zenith. Outside the atmosphere at an average distance of Earth from the sun light is 127,000 lux. The light intensity of the sun is 2,84 o10527 candles. The amount of energy coming in one minute on an area of 1 cm, as set perpendicular to the sun's rays outside the atmosphere at an average distance of Earth from the sun, called solar constant. Total capacity of solar radiation - 3,83 o10526 watts, of which the Earth goes around 2o10517 watts, the average brightness of the sun's surface (under the supervision outside the Earth's atmosphere) is 1,98 o1059 nt, the brightness center of the disk of the Sun - 2,48 o1059 nt. The brightness of the solar disk decreases from center to edge, and this decrease depends on the wavelength, so that the brightness at the edge of the solar disk for light with a wavelength of 3600A is 0,2 luminance of its center, and for the 5000A - about 0.3 brightness center of the disk of the Sun . At the very edge of the solar disk brightness decreases by 100 times for less than one second of arc, so the boundary of the solar disk looks very sharp.

Spectral composition of light emitted by the Sun, ie the distribution of energy in the center of the Sun, roughly corresponds to the distribution of energy in a blackbody radiation with a temperature of about 6000 K. However, in some parts of the spectrum there are significant deviations. The maximum energy in the solar spectrum corresponds to a wavelength of 4600 A. Solar spectrum - a continuous spectrum, which imposed no more than 20 thousand absorption lines. More than 60% of them identified with spectral lines of known chemical elements by comparing the wavelengths and relative intensity of the absorption lines in the solar spectrum with laboratory spectra. The study of absorption lines provides information not only on the chemical composition of the solar atmosphere, but also about physical conditions in those layers, which produce certain absorption. Predominant element in the Sun is hydrogen. Number of helium atoms is 4-5 times smaller than hydrogen. The number of atoms of all other elements combined, at least 1000 times less than the number of hydrogen atoms. Among them are most abundant oxygen, carbon, nitrogen, magnesium, iron and others. In the solar spectrum can be identified as lines belonging to certain molecules and free radicals: OH, NH, CH, CO and others. Magnetic fields on the Sun are measured mainly by the Zeeman splitting of absorption lines in the solar spectrum. There are several types of solar magnetic fields. Total magnetic field of the sun is low and reaches a strength of 1 of this or another polarity and varies with time. This field is closely related to the interplanetary magnetic field and its sectoral structure. Magnetic fields associated with solar activity, can reach in sunspots tension in several thousand. The structure of magnetic fields in active regions is very complicated, alternating magnetic poles of different polarity. There are also local magnetic field with the field in the hundreds outside of sunspots. Magnetic fields penetrate into the chromosphere and the solar corona. Large role in the Sun play magnetogasdynamic and plasma processes. At a temperature of 5000 - 10000 K ionized gas is enough, its conductivity is great and thanks to the huge scale solar phenomena significance of electromechanical and magnetomechanical interaction is very large.

Answer 5

The three parts of the sun's atmosphere are the photosphere, chromosphere, & corona.

Answer 6

photosphere, chromosphere, and corona are the suns atmoshere made up of (=