Big Bang Light Elements

Elements with atomic numbers greater than iron’s atomic number form during the formation of a supernovae, also known as a mini-bang. The process begins when a massive star has depleted its supply of magnesium and silicon, and only has a bare iron ore remaining. Now, the star no longer has the energy to maintain its immense mass against the force of gravity, and as a result, the entire star collapses. This process fuses together electrons and protons in the core, which forms neutrons. After neutrons build up in the ore, the star recoils in the form of an explosion. During the explosion, the neutrons attach to iron atoms in the ore, and begin converting back to protons and electrons. As a result, iron atoms are able to become different elements with greater atomic numbers.

According to Carolyn Ruth, author of “Where Do Chemical Elements Come From,” chemical elements came from the explosion of stars, also known as supernovas. In her article, Carolyn states that a newborn star is mainly composed of the first element on the periodic table, Hydrogen. Due to the high pressure within the star, a fusion process begins that fuses two protons and two neutrons together to form the second element, Helium. These fusion processes continue to form elements that weigh less than Iron. Once the star creates all elements up to Iron, the star eventually collapses and explodes. One article that agrees with Carolyn’s theory is “The Origin of the Elements and the Life of A Star”. According to this article, stars produce nuclear reactions

Carbon has six total electrons; two of the electrons it has are in its first electron shell while the other four are its valence electrons. Due to its four valence electrons, it rarely gains and/or loses electrons and/or form ionic bonds due to the fact it would have to give away or take four other electrons. In order to complete its outer shell, carbons shares its valence electrons with other atoms by having four separate covalent bonds. The carbon atom then becomes the crossing point where each molecule branches off into four separate directions.Carbon’s electron configuration allows it to bond frequently with oxygen, hydrogen, nitrogen, and phosphorus. If the carbon atom forms only a single covalent bond, The electrons form so that its bonds angle towards an imaginary tetrahedron.

“Just because you can’t see something doesn’t mean it isn’t there. It’s just waiting for the right time to show itsellf by- Emma Hart.” The atoms in our bodies and the environment around us came from a nuclear fusion, where heavier elements are made by fusing smaller atoms together.

After a star lives for about 1 million years, it becomes a main sequence star. Once it becomes a main sequence star, it will then go through a proton-proton chain reaction. Since the force of gravity goes inward, the force of fusion will then go outward from the core. This process will continue for about 10 billion years even when the star is "burning" Over those ten years, the stars will eventually slowly run out of hydrogen. After it runs out of hydrogen, the core will fill up with helium.

In the video of " We are stardust harvesting starlight" by Kraus, Tyson, and Sagan, it was mentioned that every atom present in the universe came from the explosion of a star. The collapse explosion of an unstable heavy star introduced the elements carbon, hydrogen, nitrogen and oxygen which is required to form life on earth. A statement "Forget Jesus, the stars died so that you could be here" meant that instead of looking at the religious point of view of how living forms arrived on earth, it is essential that the scientific perspective of the arrival of life forms is considered. Stars are exploded due to factors of pressure and temperature in order to release necessary elements which are the building blocks of life. The elements are a part

During the creation of stars, denser nuclei were generated from hydrogen and helium through the continuous procedure of stellar nucleosynthesis. Stars make fresh elements in their nuclei by enfolding elements together in a procedure known as nuclear fusion. Stars join hydrogen atoms to helium, then the Helium atoms are fused to generate beryllium, this process goes on, till blend in the core of star has generated each component up to iron. Nuclear fusion occurs in the hydrogen gas in the center of the Sun. It becomes squeezed together so firmly and four hydrogen nuclei join to develop one helium molecule. In the procedure, a number of-of the mass of the hydrogen atoms gets changed to energy in the formula of light. The similar procedure

The atoms are bound by shared electrons in a covalent bond. Even though they share electrons, they do not share them equally. Even though most of the time covalent bonding occurs between nonmetals, there have been times where this type of bonding occurs between a metal and a non metal. Covalent bonds are most likely to occur when molecules have a similar electro negativity level (Gray 76). Elements follow the octet rule because they are the most stable when they have eight electrons in their outer shell. Therefore, by sharing those electrons they fulfill the octet rule and the noble gas configuration. Another way covalent bonds satisfy the octet rule is too form single, double, and triple bonds. It’s easy to differentiate between those bonds, for example a single bond is when two atoms share one pair of electrons, a double bond is when two atoms share two pairs of electrons, and a triple bond is when two atoms share three pairs of electrons. Bond order and length are used to describe the strength of covalent bonds; they both have a direct relationship. Bond order is the amount of bonded pairs between two atoms. Bonding length is the distance between two covalent bonds. Compared to ionic bonds, covalent bonds are have a lower melting and boiling point. They are also less likely to dissolve in water. Not all the pairs of the molecules have the same characteristics. When a pair is not sharing any electrons, that pair is called a lone pair. When a pair is sharing electrons, they are called a bond pair. And finally, a Lewis dot structure is a great way to illustrate a covalent

The first process every star goes through before its end is the process of their core shrinking. When stars of at least .4 M begin to exhaust their hydrogen supply, the hydrogen starts to fuse in a shell that is outside the helium core. As the shell burns more hydrogen it is also producing more helium, this allows the core to increase in its mass and temperature. When the temperature increases greatly, helium fusion begins to start in what is called a helium flash, causing the star to rapidly decrease in its size and increase its temperature. Once the star has fused all of the helium out of its core, the product of the carbon will fuse which produces a hot core along with the outer shell made up of fusing helium. The more massive a star is,

The observation of the behaviour of various gaseous elements, lead to the discovery that several of them are made up of molecules, rather than atoms. An example of this would be hydrogen (H2) and oxygen (O2). Oxygen is made up of two hydrogen atoms and one oxygen atom. When these elements are bonded, they produce H2O (H2+O2 = H2O). Ionic bonds are created when one atom gives its electrons to the other atom and therefore becomes positively charged whilst the other one is negatively charged. The two atoms then attract to each other and bond. A covalent bond is formed when two atoms overlap their outer electron shell with each other. In this way, some of the electrons are shared between them. The final type of bonding is known as a metallic bond.

When such a massive star consumes all its nuclear fuel, it undergoes a 'supernova' explosion and most of the matter is expelled. The extreme heat generated during such explosions can form elements heavier than iron through nuclear fusion.

is the process of combining the nuclei of smaller atoms(less protons & neutrons and hence, a smaller atomic number) to create a larger atom. In many stars, the process starts with hydrogen (H) atoms combining to form helium atoms (He) then combining again to form Beryllium (Be) atoms and so on... The process stops when all the atoms are converted to Iron (Fe) and the star is thus dead. The reason for this is that once the atoms reach Iron and higher, the energy required to fuse the atoms becomes greater than the energy released by the atoms.

The world is made up of elements, from the iron in our blood, to the oxygen and carbon in the air. We use these elements everyday of our lives, even when we don’t realize it. But the one question that never crosses our mind is – Where do all the elements come from? Many may answer that these elements came from the Earth, but how did these elements end up on Earth? First, we have to look at the star cycle.

All substances are made of tiny particles called atoms. An element is a substance that is made of only one sort of atom. There are about 100 different elements. These are shown in the periodic table, which is a chart with all the elements arranged in a particular way. The horizontal rows in the periodic table are called periods and the vertical columns are called groups. The elements in a group have similar properties to each

Indecent bodies like the sun. Stars are made up of big exploding balls of gas, mostly hydrogen and helium. The sun is similarly a star made up of huge amounts of hydrogen, undergoing a continuous nuclear reaction like a hydrogen bomb. Stars come about when vast clouds of hydrogen, helium and dust contract and collapse due to gravity. The clouds came from astronomical plasma from “The Big Bang”, but the dust comes from the supernovae of other stars.