Sunday, June 23, 2019
Atmosphere of stars
So far, you have learned classification and famous equation of Saha based on the spectrum of stars. In this article in the 'Basic Basics of Astrophysics' series, we are going to discuss the atmosphere of beautiful stars in the sky. According to the ionization theory, we try to know what happens in a stellar environment.
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Atmosphere of stars
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We know that by the presence of a particular element in a star's atmosphere, it emerges from some specific lines in the spectrum of that star which is clear in the above picture. It depends not only on the structure of that star, but also its stellar temperature. In this article, we will try to know how using the theory of organizational theory, astrophysicist scientist knows the inner structure of that star only by seeing the spectrum of that star. We will also see how spectral classification of stars is based on the ionization theory. First of all, know what is ionization energy?
What is ionization energy?
Minimum energy ionization is called energy to remove external electrons from a metallic gas from atom. Ionization energy of some elements is high, whereas some metals have low ionization energy. The diagram below shows the deviation in energy in the ionization of various elements.
The ionization theory has paved the way for "age of imagination" to move towards "age of experimental science". This theory has proved to be the form of temperature-based sequence in the class from the O class of H. Now look at the structure and temperature of the stars on the basis of ionization theory. First, divide the stars into two categories and they understand the ionization process.
Low-temperature stars
Only coldest stars can create spectral bands related to molecules. These molecules can be hydrocarbons (CH), cyanogen (CN), carbon atom, titanium oxide (TiO) etc. These molecules can remain broken only in a cooling atmosphere. Therefore, red and yellow stars, whose surface is low on the surface, these molecules have spectrum showing lease.
Ionization of metals and stimulation energy is low. Soft stars have enough energy to stimulate these metallic lines. Therefore, the spectrum of stars with lower temperatures is the lines representing natural metals.
High-temperature stars
Now we go towards the spectrum of stars with high temperatures from low temperatures. These nostril metallic spectral lines become weak, while the ionized metal line becomes deep. The metal is partly ionized at high temperatures behind it. For example, the spectrum line of calcium-I is visible in cold M stars, while the spectrum line of calcium II is found in hot K or G strings.
Ionization energy of Hilium is the highest in relation to Hilium lines. Therefore, the helium spectrum lines are visible in stars with high temperatures. Hilium I's lines are visible in stars of class B, such as high-temperature stars.
Rectangular and ionized hilium, oxygen, carbon, nitrogen and neon lines with different ionization states are visible only in stars of O.
Author's message
Previously, the purpose of this article was to introduce the stellar environment. In its previous article, we saw the importance of breaking the mysteries of the stars in the universe by Saha equation. Research in stellar environments is the subject of more work in astrophysics. This is a broad subject and for this, information about plasma physics is necessary. In this article we have only seen the introduction of star environments. We will stop the discussion on this topic and go ahead in the series. We believe that these two articles were tough and complex, but this is the backbone of astrophysics.