A star It is an astronomical object composed of gas, mainly hydrogen and helium, and kept in equilibrium thanks to the force of gravity, which tends to compress it, and the pressure of the gas, which expands it..
In this process, a star produces immense amounts of energy from its core, in which there is a fusion reactor that synthesizes helium and other elements from hydrogen..
In these fusion reactions, the mass is not fully conserved, but a small portion is converted to energy. And since the mass of a star is enormous, even when it is one of the smallest, so is the amount of energy it gives off per second.
The main characteristics of a star are:
-Mass: highly variable, being able to be from a small fraction of the mass of the Sun to supermassive stars, with masses several times the solar mass.
-Temperature: is also a variable quantity. In the photosphere, which is the luminous surface of the star, the temperature is in the range of 50000-3000 K. While at its center it reaches millions of Kelvin.
-Colour: closely related to temperature and mass. The hotter a star is, the bluer its color and conversely, the colder it is, the more it tends towards red..
-Brightness: it depends on the power radiated by the star, which is usually not uniform. The hottest and largest stars are the brightest.
-Magnitude: is the apparent brightness they have when seen from Earth.
-Movement: stars have relative motions with respect to their field, as well as rotational motion.
-AgeStars can be as old as the universe - about 13.8 billion years - and as young as 1 billion years old.
Stars are formed from the gravitational collapse of huge clouds of cosmic gas and dust, the density of which constantly fluctuates. The primordial material in these clouds is molecular hydrogen and helium, and also traces of all known elements on Earth..
The movement of the particles that make up this huge amount of mass scattered in space is random. But from time to time the density increases slightly at one point, causing a compression.
The pressure of the gas tends to undo this compression, but the gravitational force, the one that pulls the molecules together, is a little higher, because the particles are closer together and then counteracts this effect..
Furthermore, gravity is responsible for increasing the mass even more. And as this happens, the temperature gradually increases.
Now imagine this condensation process on a large scale and with all the time available. The force of gravity is radial and the cloud of matter thus formed will have a spherical symmetry. It is called protostar.
In addition, this cloud of matter is not static, but rather rotates rapidly as the material contracts..
Over time, a core will form at very high temperature and enormous pressure, which will become the star's fusion reactor. This requires a critical mass, but when it happens, the star reaches equilibrium and thus begins, so to speak, its adult life..
The type of reactions that can occur in the nucleus will depend on the mass that it initially has, and with it the subsequent evolution of the star..
For masses less than 0.08 times the mass of the Sun - 2 x 10 30 kg approximately - the star will not form, since the nucleus will not ignite. The object thus formed will gradually cool down and the condensation will slow down, resulting in a brown dwarf.
On the other hand, if the protostar is too massive, it will also not achieve the necessary balance to become a star, so it will collapse violently.
The theory of star formation by gravitational collapse is due to the English astronomer and cosmologist James Jeans (1877-1946), who also proposed the theory of the steady state of the universe. Today this theory, which holds that matter is continually created, has been discarded in favor of the Big Bang theory..
As explained above, stars are formed by the condensation process of a nebula made of cosmic gas and dust..
This process takes time. It is estimated that it happens between 10 and 15 million years, while the star acquires its final stability. Once the pressure of the expansive gas and the force of compressive gravity are balanced, the star enters what is called the main sequence.
According to its mass, the star is located on one of the lines of the Hertzsprung-Russell diagram or H-R diagram for short. This is a graph showing the different lines of stellar evolution, all dictated by the mass of the star.
In this graph, the stars are ranked according to their luminosity based on their effective temperature, as shown below:
The main sequence is the roughly diagonal region that runs through the center of the diagram. There, at some point, the newly formed stars enter, according to their mass.
The hottest, brightest, and most massive stars are at the top and left, while the coldest and smallest stars are at the bottom right..
Mass is the parameter that governs stellar evolution, as has been said several times. Indeed, very massive stars use up their fuel quickly, while small, cool stars, such as red dwarfs, manage it more slowly..
For a human being, red dwarfs are practically eternal, no known red dwarfs have died yet.
Adjacent to the main sequence are the stars that, due to their evolution, have moved to other lines. In this way, above are the giant and supergiant stars, and below the white dwarfs..
What comes to us from distant stars is their light, and from its analysis a great deal of information is obtained about the nature of the star. At the bottom of the H-R diagram is a series of letters denoting the most common spectral types:
O B A F G K M
The stars with the highest temperature are O and the coldest are class M. In turn, each of these categories is divided into ten different subtypes, differentiating them by a number from 0 to 9. For example, F5, an intermediate star between F0 and G0.
The Morgan Keenan classification adds the luminosity of the star to the spectral type, with Roman numerals from I to V. In this way, our Sun is a G2V-type star. It should be noted that given the great variability of stars, there are other classifications for them.
Each spectral class has an apparent color, according to the H-R diagram in the figure. It is the approximate color that an observer would see without instruments or at most binoculars, on a very dark and clear night.
Here is a brief description of its characteristics according to the classical spectral types:
They are blue stars with violet hues. They are found in the upper left corner of the H-R diagram, that is, they have large size and luminosity, as well as high surface temperatures, between 40,000 and 20,000 K.
Examples of this type of star are Alnitak A, from the belt of the constellation Orion, visible during the nights of northern winter, and Sigma-Orionis in the same constellation..
They are blue stars with surface temperatures between 20,000 and 10,000 K. A star of this type that is easily visible to the naked eye is the giant Rigel, which is part of a star system in the constellation Orion..
They are easy to see with the naked eye. Its color is white-blue, with surface temperatures between 10,000 -7000 K. Sirius A, a binary star in the constellation Canis Major, is a type A star, as is Deneb, the brightest star in the Swan..
They look white tending to yellow, the surface temperature is even lower than those of the previous type: between 7000 and 6000 K. The polar star Polaris, from the constellation Ursa Minor belongs to this category, as well as Canopus, the brightest star of the constellation Carina, visible far to the south of the northern hemisphere, during the northern winter.
They are yellow and their temperatures are between 6000 and 4800 K. Our Sun falls into this category..
Their color is yellow-orange, due to their lower temperature range: 4800 - 3100 K (giant K0). Aldebaran in Taurus, visible during the northern hemisphere winter, and Albireo de Cisne, are good examples of K-type stars..
They are the coldest stars of all, presenting a red or orange-red coloration. The surface temperature is between 3400 and 2000 K. Red dwarfs fall into this category, as well as red giants and supergiants, such as Proxima centauri (red dwarf) and Betelgeuse (red giant) of the constellation Orion..
In principle, it is not easy to find out the internal structure of a star, since most of them are very distant objects..
Thanks to the study of the Sun, the closest star, we know that most stars are made up of gaseous layers with spherical symmetry, at the center of which there is a core where the fusion takes place. This occupies more or less 15% of the total volume of the star.
Surrounding the nucleus there is a layer like a mantle or envelope and finally there is the atmosphere of the star, whose surface is considered its outer limit. The nature of these layers changes with time and the evolution followed by the star.
In some cases, at a point where hydrogen, its main nuclear fuel, runs out, the star swells and then expels its outermost layers into space, forming what is known as a planetary nebula, in the center of which the bare nucleus remains. , hereinafter known as a white dwarf.
It is precisely in the envelope of the star, where the transport of energy from the core to the outer layers takes place.
In the section devoted to spectral types, the types of stars that are currently known have been mentioned very generally. This in terms of the characteristics discovered through the analysis of its light.
But throughout their evolution, most of the stars move on the main sequence and also leave it, locating in other branches. Only red dwarf stars remain in the main sequence their entire lives.
There are other types of stars that are mentioned frequently, which we briefly describe:
It is a term used to describe very different types of stars, which on the other hand have their small size in common. Some stars are formed with very low mass, but others that were born with much greater mass, instead become dwarfs during their lifetime..
In fact, dwarf stars are the most abundant kind of star in the universe, so it is worth dwelling a bit on their characteristics:
They are protostars whose mass was not enough to start the nuclear reactor that propels a star into the main sequence. They can be considered to be halfway between a giant gas planet like Jupiter and a red dwarf star..
Since they lack a stable energy source, they are destined to cool down slowly. An example of a brown dwarf is Luhman 16 in the constellation Vela. But this does not prevent the planets from orbiting them, since so far several have been discovered.
Their mass is small, less than that of the Sun, but their life passes in the main sequence because they carefully spend their fuel. For this reason they are also colder, but they are the most abundant type of star and also the longest of all.
It is the remnant of a star that left the main sequence when the fuel in its core ran out, swelling until it became a red giant. After this, the star sheds its outer layers, reducing its size and leaving only the core, which is the white dwarf..
The white dwarf stage is only one phase in the evolution of all stars that are neither red dwarfs nor blue giants. The latter, being so massive, tend to end their life in colossal explosions called nova or supernova.
The star IK Pegasi is an example of a white dwarf, a fate that may await our Sun many millions of years from now..
They are hypothetical stars, that is, their existence has not yet been proven. But it is believed that red dwarfs eventually transform into blue dwarfs when they run out of fuel..
They are ancient white dwarfs that have completely cooled down and no longer emit light..
This is sometimes the name given to stars with a mass comparable to or less than that of the Sun, but greater in size and temperature than red dwarfs.
This is the last stage in the life of a supergiant star, when it has already used up its nuclear fuel and suffers a supernova explosion. Due to the explosion, the core of the remaining star becomes incredibly compact, to the point where electrons and protons fuse to become neutrons..
A neutron star is so, so dense, that it can contain up to twice the solar mass in a sphere about 10 km in diameter. Since its radius has decreased so much, conservation of angular momentum requires a higher rotational speed.
Due to their size, they are detected by the intense radiation they emit in the form of a beam that rotates rapidly next to the star, forming what is known as a press.
Although stars have characteristics in common, as with living things, the variability is enormous. As has been seen, there are giant and supergiant stars, dwarfs, neutrons, variables, of great mass, of enormous size, closer and more distant:
-The brightest star in the night sky is Sirius, in the constellation Canis Major.
-Proxima Centauri is the closest star to the Sun.
-Being the brightest star does not mean being the brightest, because distance counts for a lot. The most luminous star known is also the most massive: R136a1 belonging to the Large Magellanic Cloud.
-The mass of R136a1 is 265 times the mass of the Sun.
-The star with the greatest mass is not always the largest. The largest star to date is UY Scuti in the constellation of the Shield. Its radius is approximately 1708 times larger than the radius of the Sun (the radius of the Sun is 6.96 x 10 8 meters).
-The fastest star so far had been US 708, which is moving at 1200 km / s, but recently another star was discovered that surpasses it: S5-HVS1 of the constellation Crane, with a speed of 1700 km / s. It is believed that the culprit is the supermassive black hole Sagittarius A, in the center of the Milky Way..