How the universe was created? How does the story become a place that seemslimitless we know to this day? And what will happen after this time? Before continuing your reading activities, help us to click the image on the side. This is a question that has puzzled philosophers and scholars since the beginning oftime, and led to some pretty wild and interesting theories. Currently, theconsensus among scientists, astronomers and kosmolog is that the universe as we know it was made in a large explosion that not only creates the majority ofthe material, but the laws of physics that governs our cosmos is constantly evolving.
This is known as The Big Bang theory. For nearly a century, the term has becomethe fruit of the mouth of scholars and non-scholars. This theory has come in andbe accepted, see the theory as the basis of the initial assumptions about theformation of the universe. But what exactly does that mean? How our universein the big bang, what evidence is there today, and what the long term theory to our universe?
The basics of the theory is quite simple. In short, the Big Bang hypothesis States that all material present and past in the universe arose at the same time, about 13.8 billion years ago. At this point, all the material is compacted into a ball thatis very small with infinite density and great heat is called the Singularity.Suddenly, the Singularity is starting to develop, and the universe as we know itrebooted.
Although this is not the only modern theories of how the universe came into being for example, there is the Steady State Theory or the theory of OscillatingUniverse – it is the most widely accepted and popular. Not only does the modelexplains the origin of all matter are known, the laws of physics, and the large scale structure of the universe, also contributed to the expansion of the universeand the various other phenomena
Timeline:.
Working backwards from the current state of the universe, scientists havetheorized that it must have come at one point of infinite density and the limited time that began to develop. After the initial expansion, the theory States that the universe cooled enough to allow the formation of Atomic and subatomic particles, then simple. A giant cloud of primordial elements then rallied throughgravity to form stars and galaxies.
This all started about 13.8 billion years ago, and thus considered the age of the universe. Through the testing of theoretical principles, an experiment involvingparticle accelerators and high-energy astronomy studies, and who have observed the deep universe, scientists have constructed a timeline of events thatbegan with the Big Bang and has led to the current state of cosmic evolution.
However, the early universe--which lasted from about 10-43sampai 10-11detikafter the Big Bang — is the subject of widespread speculation. Given that thelaws of physics as we know them could not exist at the moment, it is difficult to imagine how the universe could have been arranged. Moreover, experimentsthat can create the kind of energy that is involved is not yet done. However,many theories applicable to what happens at the beginning of this instant in time, many
Singularity:
Also known as the Planck Epoch (or Planck Era), this is the earliest known periodof the universe. At the moment, all the material that condensed on a single point of infinite density and extreme heat. During this period, believed thatquantum gravity effects dominate the physical interaction and that no otherphysical strength from the power equal to gravity.
Planck is a period of time extending from point 0 to 10-43detik, and was so named because it can only be measured in Planck time. Because of the extreme heat and density of matter, the universe is very unstable. Thus began to expandand cool, which leads to the realization of the basic forces of physics.
From about 10-43 second and 10 -36, the universe began crossing the transition temperature. It is here that the fundamental forces that govern the universe is believed to have begun to separate from each other. The first step in this is the force of gravity separates from the gauge, which takes into account the strong and weak nuclear forces, and electromagnetism.
Later, from 10-36sampai 10-32detik after the Big Bang, the temperature of the universe is low enough (1028K) that the power of electromagnetism (strong force) and the weak nuclear force (a weak interaction) are able to separate too,forming two power berbedaEpoch:.
Inflation
With the creation of the first fundamental forces of the universe, the inflationEpoch began, lasting from 10 to 32detik within Planck to the unknown point.Most cosmological models shows that the universe at this time filled withhomogenized density high energy , and that a very high temperature and pressure gave rise to the rapid expansion and cooling.
It starts at 10-37detik, where phase transitions which led to the separation offorces has also contributed to the period in which the universe grewexponentially. It was also at this point in time the Baryogenesis to occur, which refers to a hypothetical event where the temperature is so high that the randommotions of particles occur at relativistic speeds.
As a result of this, the particle-antiparticle pairs of all kinds were beingcontinuously created and destroyed in the collision, which is believed to have led to the dominance of the material more antimatter in the universe. Afterinflation stopped, the universe consisted of a quark-gluon plasma, as well as allother elementary particles. From this point onwards, the universe started to cooland caring come together and make Epoch:.
Cooling
As the universe continued to decrease in density and temperature, the energy ofeach particle starts to diminish and the transition phase continues until the fundamental forces of physics and elementary particles are transformed into its present form. Since the energy of the particle will fall to values that can be obtained with particle physics experiments, this period onwards incur lessspeculation.
For example, scientists believe that about 10-11detik after the Big Bang, the energy of the particles go down much. At about 10-6 seconds, quarks andgluons form Baryons such as protons and neutrons, and little more quarkantiquark excess causes an excess of small baryon more antibaryons.
Because the temperature is not high enough to create new proton-antiprotonpair (or pairs of neutron-anitneutron), mass annihilation immediately followed, leaving only one of the original protons and neutrons are 1010dari and no their antiparticles. A similar process occurs in approximately 1 second after the Big Bang to electrons and positrons. After these annihilations, the remainingprotons, neutrons and electrons were no longer moving relativistically and the energy density of the universe was dominated by photons-and at a lower rate,neutrinonukleosintesis.
A few minutes into the expansion, a period known as the Big Bang also began.Thanks to the temperature down to 1 billion kelvins and the density of energydropping approximately the equivalent of air, neutrons and protons joined to form the universe's deuterium (Hydrogen stable isotopes) and helium atoms.However, the majority of the protons the universe remained uncombined as hydrogen nuclei.
After approximately 379,000 years, this core combined with electrons to form atoms (again, mostly hydrogen), while the radiation decoupled from matter and continued to flourish through space, mostly without a hitch. This radiation is now known what is the Cosmic Microwave Background (CMB), which today isthe oldest light in the universe.
As CMB expanded, gradually lose energy and density, and is currently estimated to have a temperature of 2.7260 ± 0.0013 K (-270,424 ° C/454.763 ° F) and the energy density of 0.25 eV/cm3 (or 4.005 × 10-14J/m3; 400-500 photons/cm3). CMB can be seen in all directions at a distance of about 13.8 billion light years, but estimates place the actual distance was about 46 billion light years from the center of natural semestaEpoch:.
The structure of the
Over the last few billion years that followed, the area is slightly denser than the material almost evenly from the universe of gravity starts to become attracted to each other. Therefore they grew even denser, forming gas clouds, stars, galaxies, and the other astronomical structures which we regularly observe now.
This is what is known as the structure of the Epoch, because it was during this time that the universe began to form. It consists of material that is distributed within the structure visible from a wide variety of sizes, ranging from stars and planets to galaxies, clusters of galaxies, and super clusters – where the materialis concentrated.
Separated by a very large Bay which contains some galaxies
The details of this process depend on the amount and type of matter in the universe, the material with a cool dark, warm dark matter, hot dark matter,Baryons and substances into four types are recommended. However, models ofLambda-Cold Dark Matter (Lambda-CDM), in manapartikel-partikelmaterigelapbergerak slowly compared to the speed of light, is considered as the standard model of the Big Bang cosmology, since it best fits the available data.
In this model, dinginmateri gelapdiperkirakan makes about 23% of matter/energy of the universe, while the substance of Baryons made up about4.6%. The Lambda refers to the Cosmological Constant, a theory initiallyproposed by Albert Einstein who attempted to show that the balance of mass-energy in the universe was static. In this case, this is related to Dark Energy, which served to accelerate the expansion of the universe and keep large scalestructure especially seragampanjang.
Long-term prediction
Flood hypothesis
The 1990s also saw the emergence of Dark Energy as an attempt to resolve the outstanding issues in cosmology. In addition to providing a description of the missing mass of the universe (along with Dark Matter, originally proposed in 1932 by Jan Oort), also gave an explanation of why the universe is stillaccelerating, as well as offering a resolution to Einstein's cosmological constant.
Significant progress made thanks to advances in telescopes, satellites, andcomputer simulations, which has allowed astronomers and kosmolog to see more semestaalamdan get a better understanding of actual age. Introduction tospace telescope-like Cosmic Background Explorer (COBE), the Hubble Space Telescope, the Wilkinson Microwave Anisotropy Probe (WMAP) and PlanckObservatory also has the value.
Today, kosmolog has a fairly precise measurements and the many parameters of the Big Bang model, not to mention the age of the universe itself. And it all began with the observation noted that big star objects, light years away, slowlyslipping away from us. And while we are still not sure how it all will end, we know that on a cosmological scale, it's not going to be a long, long time!
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