Neutron Stars Research Paper

When stars died, chemicals other than hydrogen and helium formed, which led to the next level of complexity—Heavier Chemical Element. Most stars spent about 90% of their life over billions of years on during protons and hydrogen nuclei into helium nuclei. When they run out of fuel, the furnace at the center of the star stopped supporting the star, and gravity took over. Small stars did not have much pressure at the center. They burned hydrogen slowly over billions of years at relatively low temperatures. When they died, they would slowly fade away. However, great stars had so much mass that they can create enormous pressures and temperature, and when the giant stars ran out of hydrogen, the temperature got cranked up even higher, which led the star to collapse. The high temperature that the collapse caused was able to make helium nuclei fuse into nuclei of carbon. When a star used up its helium, it collapsed again, and the cycle started over. The star heated up and began to fuse carbon to form

As this slow contraction continues, the core temperature, density, and pressure of the star continues to increase. As the star shrinks it becomes so dense that it starts to compress helium. This results in the star to swell due to the hot core and leaving a relatively cool surface. Eventually the outer layers of the star expand outwards, increasing the size of the star. As the layers continue to expand, the surface temperature continues to cool, forming a relatively large star called a red giant.

Orion has two of the brightest stars, be Betelgeuse and Rigel. Betelgeuse is a red supergiant. The gravity of the star squeezes its core tightly, heating it to billions of degrees. It then fuses the helium to make heavier elements. When that happens, the star no longer produces energy in the core. Without the reactions in its core to push outward, gravity quickly causes the core to collapse, forming a neutron star.

The larger a star, the shorter their lifespan is, and they explode as supernovae, blasting out powerful shockwaves that create a chain-reaction that spews throughout the galaxy. Within just a few million years, the galaxy is forming stars up to hundreds of times more than a normal galaxy would. When all of the gas available is used up in about ten million years, the galaxy calms down and the period

Soon Mason felt he was ready, so he exploded! After Mason exploded into a supernova, his mass compressed him into a neutron star. Mason then lived a long and happy life as a neutron star, until one day. On one eventful day, a neighboring neutron star, named HeavenLea got a little too close to Mason and they started spinning very fast, pulled together by gravity. Until eventually, Mason and HeavenLea crashed, creating even more heat and pressure than a normal supernova! This crash resulted in some of the strongest elements like

The neutron star is composed of the combination of both electron and protons that will develop into purely neutrons, which make up the core (Astronomy 2016). The density of neutron stars is so

During the condensing of the star’s core, the neutrinos are able to escape, but the neutrons are squished together so much that their density is the same of an atomic nucleus’ density. A violent explosion happens during this process and its called a “supernova”. To put this into perspective, imagine taking something the size of our sun, if not bigger, and compacting it into an area the size of a city. This is so dense that just a teaspoon of it would weigh about 1 billion tons! Crazy, right?

Our Sun is not large enough to become a black hole when it dies. When the Sun loses all of its available nuclear fuel in its core, the Sun will die a quiet death. Stars that have the same size as the Sun are called Solar Mass Stars. When a Solar Mass star dies, its remnants become a white dwarf. Stars that have more mass will eventually become a black hole when they die. When a massive star loses all of its fuel, it is not able to sustain its own weight anymore and begins to collapse on itself. The massive star begins to heat up and a fraction of the stars outer layer. The massive stars outer layer also contains fresh nuclear fuel. This activates the nuclear reaction again and an explosion called a super nova happens. The innermost part of the massive star, the core, still continues to collapse. Depending on the size of the stars core, the star might become a neutron star and the collapsing stops or it will keep on continuing to collapse into a black hole. The dividing mass of the stars core is what determines the stars

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.

Supernovas are the explosion of a star when it reaches the end of its life. There are two ways a star can go supernova. The first way or a Type I supernova occurs in the Binary system which is when two stars orbit the same point. The two stars are a white dwarf and a red giant. A white dwarf is a small dense star that is around the size of a planet and a red giant is a star at its last stages of life. If these two stars are close enough, matter will be transferred to the white dwarf from the red giant. When the star’s core reaches its limit of matter, a thermonuclear detonation will occur leaving nothing behind unless there were leftover elements in the white dwarf or there were elements made in the supernova explosion. One of the elements made in the explosion is radioactive nickel.

The force pushing out of the star and gravity become unbalanced. In the life of a star there is a balance between force pushing out of the star and gravity pulling in. When the force pushing out escapes, the gravity collapses on the rest of the star. (“HubbleSite - Reference Desk”) After the Gravity collapses it compresses the core into such a small space where the gravity is so strong, that is the black hole the gravity is so strong that not even light can escape. (“How Do Black Holes Form?”) That is what causes large stars to collapse and create black

Stars are massive balls of fire that can produce heat up to 6,000 Kelvin. In the process of nuclear fusion elements are combined in order to create heavier elements. As a result, massive amounts of energy is created. This energy is then used by the sun to keep itself intact. Nuclear fusion forged helium atoms through the fusion of hydrogen atoms in the center of stars. The process of combining lighter elements to form heavier elements continues making elements like oxygen and silicon. However, nuclear fusion can only occur to a certain extent. Thus the heaviest element a star can produce is iron because a star is unable to move heavier particles to make energy. As a result of fusing heavy elements, the star becomes unable to create the amount of energy needed for stability, and it

They are larger and cooler with temps ranging from 3,500- 4,500K. When fusion of helium is rapid, the star expands. When fusion is slow, the star may condense and form a blue supergiant.

When the star actually starts to run out of nuclear fuel some of the mass flows into the star's core. When the core becomes too heavy it cannot take its own gravitational force. Which causes the core to collapse, and as it collapses it results in a giant supernova. Many people worry that the sun will become into a supernova. That has no chance of happening because the sun does not have enough mass to become a supernova.

Main sequence stars like our own sun enduring in a state of nuclear fusion during which they will produce energy for billions of years by replacing hydrogen to helium. Stars change over billions of years. When their main sequence phase ends they pass through other states of existence according to their size and other characteristics. The larger a star's mass, the shorter its lifespan is. As stars move toward the end of their lives, much of their hydrogen will be converted to helium. Helium sinks to the star's core and raises the star's temperature—causing its outer shell to expand. These large, puffy stars are known as Red Giants. The red giant phase is actually a prelude to a star shedding its outer layers and becoming a small, dense body called a White Dwarf. White dwarfs cool down for billions and billions of years, until they finally go dark and produce no energy at all. Once this happens, scientists have yet to observe, such stars become known as Black Dwarfs. A few stars avoid this evolutionary path and instead go out with a bang, exploding as Supernovae. These violent explosions leave behind a small core that will then turn into something called a Neutron Star or even, if the remainder is large enough, it is then turned into something called a Black Hole.