Sunday, June 23, 2019
Sun structure
There is approximately 1 trillion stars in the Milky way. The most important star for us is Sun. This is the bright star that revolves around the Earth with other planets. Today in this article we will learn the sun very closely. In the thirteenth article of 'Basic Basics of Astrophysics' series, we will get information about the structure and structure of the sun.
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| Sun structure |
Sun is our nearest star, from which we have got more chances to learn and study this star in detail. This is the only star that we can see in the form of a disc, while the other stars look only at the point of view. Modern sophisticated equipment and efficient inspection techniques have given us the opportunity to study the actual physical properties of the sun. But we can only see the sun's atmosphere and its fierce external outings. Scientific studies of physics and the study of outer surfaces of the Sun add to its internal layers. In this article we will see a brief introduction to the structure, components and various activities of the sun.
Sun structure
In the previous article we have discussed the Hertzprung Russell Diagram (THE HERTZSPRUNG RUSSELL DIAGRAM). According to the alphabetical classification, the Sun is the star of the main sequence of the class. It is also called the yellow dwarf star informally. It has 73% hydrogen and 25% Hilium. Other heavy elements like oxygen, carbon, ni'an and iron are present inside the sun.
Different layers of the sun
The sun has both main areas, internal and external areas. The interior area is made up of solar core and subsequently radiation and convective area. Flammable processes continue in the solar system. These processes are the source of the sun's abundant energy. The area outside this intrinsic area is a solar environment, part of which is photosphere, chromosphere, transition and corona or corona.
Photosphere
It is clear from the name of this area that photosphere is the visible area of the sun. The light from this region publishes the parts of the solar environment. The next field after the photosphere in the solar system is invisible due to the intensity of the photosphere. Sunspots generated from the effects of the magnetic field on the Sun are produced in this area. The temperature of this region is between 5770 K-5780 K.
Chromosphere
Chrome means color, and according to the name of the chromosphere, this region is light pink or light red. The density of this area is extremely low, that is, 8-10 times the Earth's ocean surface environment and can only be seen at the time of solar eclipse. The temperature of this region is approximately 20,000 K.
Transition Region
The transition area comes after the chromosphere. The temperature in this area suddenly increases from 20,000 K to 1,000,000 K. This area can not be seen from Earth. But it can be easily seen by the satellites of space for sensitive ultraviolet spectral devices.
The Corona
The outermost region of the Sun is the corona or Corona. It is a spontaneous expansion of the chromosphere but it is very different from the properties. Corona can be clearly seen at the time of solar eclipse. It looks like an aura surrounded by the inner part of the sun. The outermost part of this area can be seen far from the Sun's disk till the space between the planets. Its temperature ranges from one million Kg to Kelvin. This is an anomaly. In this structure, the temperature of the source is extremely low, but how much heat does it make? How hot does the thermal heat up to a million kilograms of kelvin by passing heat from the cool photosphere of 5900 K temperature? The source of heat to the halo should be something else. One of the unsolved puzzles of astrophysicology is: The Solar Hubble's Puzzle to Be Heat.
He keeps information about the human halo for centuries but he did not know about its reality and nature. The scientists first thought it was only an illusion. Even astronomers such as Kepler were unaware of its true nature. In 1869, American astronomer W. Harkness and C. A. Young studied the spectrum of solar aura for the first time. After this, in 1930, French physicist B. Lyot took the first picture of the halo through chronograph equipment. In this area, structures like solar prominence are visible.
Author's message
Through this article, we have introduced a new branch of solar physics in the Astrophysicist article series. The author is Plasma Physicist and he has studied Alfven waves which can potentially be liable to be unusually hot due to solar aura. If you want to know the structure of the sun in depth then you must have knowledge of electrodynamics and plasma physics. In the next article of this series, we will get information about some of the properties of the sun's surface, such as solar spots, solar flares.