Understanding Large-Scale Structure of Matter Using Cosmological Modeling

The Large-scale Structure of Matter (LSM) is a theory of nature.

It postulates that all solid matter exists in far larger-sized molecular structures than can be seen by the naked eye. 

Scientists have thus decoded subtle irregularities in the observed light patterns of the early universe to map large-scale filamentous structures which serve as transport links for delivering material to more dense, highly structured hub-like structures like galaxy clusters. In these large-sized structures, the interconnected filaments are covered with matter that consists primarily of hydrogen, helium, carbon, silicon, and other atomic particles. These atoms are held together by electrostatic repulsion and gravity and their collective weight can support the entire weight of the structure.

If the large-scale structure may be infinite in nature.

It might have no beginning or end and if it has a beginning, it might have no end either. 

For example, large-scale structure of matter in the visible portion of the spectrum is composed of hot plasma, extremely heavy neutral atoms, extremely heavy molecules such as inorganic compounds, and extremely hot electrons. In case of the invisible portions, the large-scale structure could consist of hydrogen atoms, deuterium, tritium, helium, neon, and other atoms in ionized form. And last but not the least, there is the macroscopical aspect of this theory, which is the observation that there are symmetries in the structure of large-scale structure of matter in the visible portion of the electromagnetic spectrum.

The proton formed within an eddy current in a neutral field. 

Simulations also suggest that the primordial particle eventually became very heavy and that its density dominates the distribution of space-time. The present-day abundance of most of the known elements in our solar system, together with all the common elements of those primitive planets were produced in the early solar system and that they are contained in the atomic particles that constitute the protospheres of these planets. 

Consequently, the present-day solar system formed with a variety of atomic constituents from the primordial planet crust. These elements, together with several hundred millions of minor amounts, are the ingredients of our present-day atom and everything that constitutes it.

Present-day solar system and the whole cosmos are fractions of the Milky Way. 

Source: Springer

The simulations of the Milky Way disk imply that, unlike the virtual models of the early solar system, the Milky Way has a denser gas disk than can be explained by the physics of the solar system. Similarly, simulations of the supergalaxy imply that the gas disks of this space may also be quite dense and relatively more difficult to manipulate than the flat disk of the solar system. The present-day most well-known example of a galaxy is the Sagittarius spiral galaxy. Although it is not very heavy (less than half a million stars), it contains twice as many protospheres as the entire Milky Way.

In addition, the present-day astronomers have detected almost two hundred galaxies which are far more numerous than the cold stars, which are believed to form a portion of the large-scale structure of matter in the universe. Thus, astronomers have shown that a significant number (around 100 or so) of very compact elliptical galaxies are probably present along with many spirals, pulsars, and black holes. 

Unlike the Sagittarius spiral, however, the Milky Way has neither a spiral nor a hole. In addition, nearly one third of the spiral’s mass consists of dark matter, which is believed to make up most of the bulk of the universe’s substance.

The researchers from NASA have a different point of view. 

According to them, it is extremely unlikely that any of these spiral galaxies contains an earth-like planet as it is very heavy and very cool. The presence of a super-dense gas over an elliptical galaxy could indicate that there are either clouds of gas or a merging black hole inside the galaxy. Another possibility is that the gas is being heated by a red planet, which makes it glow-and thus giving out radiation that has a strong effect on our solar system. Finally, some studies have indicated that there could be another planet beyond our solar system, which could make the solar system much tidier.

The structure formation of the early universe is similar to the current structure formation.

One thing that makes the simulations so interesting is the fact that they reproduce the processes that were going on at the time of formation of the first planets in our solar system. We can use these same simulations to understand what happened to the planets and eventually to our moon and the other outer solar system bodies. It is also believed that the moon has a very stable orbit around the earth, which is not the case if the moon is thought to be more like a comet than an actual satellite. 

When you study the evolution of large-scale structure formation in the early universe, you can learn a lot from the simulations. They have made it clear that a variety of natural processes took place, but we should also be able to draw some inferences from studying the properties of matter at various temperatures.

The “halo” of space. 

This pattern of dark matter surrounds most of the rapidly moving galaxies. This form of dark matter is made of gas, dust, and stars, and it is made up of 100’s of times the density of our own atmosphere. Since the halo of space is mostly invisible and can only be seen through special telescopes, we cannot see it with the naked eye. Only by using powerful satellites that orbit around the earth and looking for dimples in the clouds can we make this connection to the larger-than-normal structures that we see around the Milky Way, including spiral arm structures and spirals.

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