La evolution of the stars It is given over millions of years. That is, these are born when a large sum of matter is collected in an area of the cosmos. The material is pressed and heated until a nuclear resistance begins, which absorbs matter, transforming it into energy. The small stars spend it lazily and last longer than the big ones.
The hypotheses about evolution of the stars they are based on successful proofs of thesis of the spectra related to radiance. Research shows that many stars can be cataloged in a usual series in which the most radiant They are the hottest, the smallest, and the coldest. Furthermore, they can be analyzed in the context of the stars as various types.
evolution of the stars
According to what was mentioned above, the evolution of the stars is given by a series of stages, these would be:
The existence of a star
The life span of a star begins like a huge mass of vapor correspondingly cold. The convulsion of the gas raises the temperature until the inner part of the star reaches 1.000.000 °C. In this part they have atomic reactions, the consequence of which is that the axes of the hydrogen particles are adjusted with those of deuterium to form helium foci. This resistance redeems vast sums of energy, and the convulsion of the star stops. For a while it seems to be fixed.
But when the emancipation of energy closes, the convulsion starts again and the temperature of the star returns to increase. At a given moment a rebellion begins between lithium, hydrogen and other light metals assisting in the body of the star. Again energy is released and the contortion stops.
When the lithium and other light raw materials are fulfilled, the contortion is renewed and the star enters the final phase of refinement in which hydrogen is converted to helium at very penetrating temperatures thanks to the catalytic exercise of carbon and nitrogen. This thermonuclear force is characteristic of the main series of stars and perpetuates until all the hydrogen that exists is exhausted. In this process, the galaxy formation It can also influence the life cycle of stars.
red giant
The star becomes a red giant and reaches its largest dimension when all of its central hydrogen has been released into helium. If it continues to glow, the temperature of the focus should scale high enough to cause the helium axes to melt. During this time it is possible for the star to become much smaller and therefore heavier.
When it has used all the viable principles of atomic verve, it constricts again and catechizes into a white dwarf. This final epoch may be sealed by frequented outbursts as "novae." When a star redeems its outer covering bursting out like nova or supernova, restores to the celestial medium a component more charged than the hydrogen that it has summarized in its internal part.
The future offspring of stars created from this element will begin their life with a richer variety of heavy compendiums than the previous reproductions. stars in clusters that are taken from their outer layers of a non-hazardous representation are Christianized into astral nebulae, ancient stars surrounded by gas globes that diffuse on a multiple scale of frequency extensions.
From star to Super Massive Black Hole
stars with a agglomeration much extraordinary than that of the Sun tolerate a more vertiginous progress, of a few million years from their origin to the explosion of a supernova star. Later, they can become black holes.
Preliminary mass: progressive state terminable
Vaporous debris from a supernova (designated remnants) spread out over a wide region of space, creating an indestructible spreading cloud that moves away at several kilometers per second and whose typologies are very specific.
The vapor that accommodates a supernova remnant is very unlike the vapor in the cloud that created the star. The initial cloud was disposed almost exclusively by helium, while in the remnant a great diversity of chemical compendia is located, remains of the nuclear fusion that happened in the star that has disappeared and of the similarly others created during the burst that originates in the supernova period. This phenomenon is studied in relation to the ancient astronomy that seeks to understand these events.
In a supernova detonation, a disastrous collapse of the star occurs; due to its large number, the formidable force of gravity presses down on the component with much greater force than in the case of a white dwarf. In these contexts, all the mass of a usual star (as is the case with our sun) is squeezed into a small sphere just 15 km in diameter; these microscopic stars have been nicknamed neutron stars.
On the other hand, the matter in these things has been squeezed to such an extent and its cohesion reaches such great values, that the Electrons combine with protons, creating new neutrons. This process can also be observed in the formation of new .
Conclusions about the evolution of stars
According to the sum and the enormous complexity of stars that are recorded, it is possible to have a representation of their evolution by noting stars in the various periods (or phases) of their presence: from their elaboration to their disappearance. In this regard, it should be considered that, positively, have been examined disappear stars (as was the case with the 1987 supernova) as well as evidence of the creation of new ones.
We have already mentioned that in the exposure of the stars, physical measures such as temperature or crowd, among others, are used. But another of the frequent methodologies in astronomy must also be determined, which is designated as Spectroscopy. This method is essential to understand the modern astronomy and the study of starlight.
The chemical elements that give the evolution of stars
Different chemical components absorb or express luminescence depending on the temperature at which they are found; in this way the representation (or estrangement) of certain components in the star's atmosphere, shows the temperature of the starThis can be studied further in the works on famous astronomers who have contributed to this field.
the hot stars
In the hottest stars, the different inner layers must command greater gravitational affinity than the outermost robes, and therefore the pressure of the vapor must be greater to maintain the size; as a result, the temperature of its interior is higher. This means that the star must "scorch" the flammable material very quickly, which generates a huge amount of energy. This type of star can only enjoy a limited life. In this sense, its study can be related to the stellar moments of humanity.
the cold stars
Cool stars (usually small and weak in gravity) only produce a humble amount of energy; in sequel they arise finely shining. A) Yes, these stars may be as such only a few billion years. When compared with the hottest stars, one can see how the possibility of life in space may depend on these stellar processes.
Now, the temperature and, consequently, the amount of cold that a star expresses, depends on its crowd, that is, the greater its mass, the higher the temperature and by resultant greater is the sum of character that it diffuses.
On the other hand, until the temperature on its axis reaches a value of a few million levels, atomic metamorphoses will not be caused (of the hydrogen to helium transformation specimen) and, consequently, until that happens, the amount of energy that they express will be very small.
Finally, when the evolution of the stars and life begins, the burning of its interior comes from the gravitational character, in other words, from the vapor cloud that is pressed into it.
