Type II Supernovae

- Because the interior of a less massive star doesn’t reach sufficiently high temperature and pressure to fuse helium. So the only energy source is hydrogen.

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

Wolf-Rayet Stars – These massive stars are evolved and have completely lost their outer hydrogen, so they are fusing helium and heavy elements in their core.

The difference between a type Ia and Type II supernova is that a type II is caused by a big star collapsing and a Ia supernova is a white dwarf that emits enough mass and power to overcome the chandraskhar limit and collapses under the weight of it’s overly increased power.

High-mass stars don’t last as long in the main sequence stage because they use their energy fastly. After millions of years, a high-mass star expands into a supergiant star. In the core of this star, fusion produces heavier and heavier elements. Then when a iron ore forms, fusion stops and the core collapses. Then parts of the core bounces outward, and the star explodes into a supernova. This explosion can form a extremely dense body called a neutron star. Sometimes a supernova leaves behind a core where it collapses forming into a invisible object called a black

First, I will discuss protostars. A protostar is a very young star that is gathering gas from a giant molecular cloud. “The protostar phase of stellar evolution lasts about 100,000 years”. (www.universetoday.com) As time goes on, pressure and gravity increase, which therefore forces tho protostar to collapse down. The energy released by the

A nebula collapses due to gravitational or magnetic disturbance. Potential energy is lost when gases collect, this causes an increase in temperature. The more it collapses the more the temperature will increase. Many stars will form due to the collapsing of a cloud that separates into many smaller clouds each of which becomes a star. The part to collapse faster than any other part is the core while the outer parts collapse at a slower rate, to conserve angular momentum the cloud begins to rotate faster and faster, the outer parts collapse slower than the core. The molecules of hydrogen gas break into hydrogen atoms when the core reaches a temperature of 2000 degrees kelvin (1726.85 degrees Celsius). It begins to look like a star when fusion reaction begins when the core reaches a temperature of 10000 degrees kelvin (9726.85 degrees

To start on how the sun produces heat, the sun consists mostly of hydrogen, especially at its core. The core is only one fourth of its size but this is where all of the reactions happen and where all the heat of the sun is actually produced. In the core of a star, it is so pressurized and so hot that nuclear fusion occurs every 9.2×1037 times a second. The hydrogen molecules are forced together to make helium molecules. When this reaction occurs, it releases 0.7% of the mass in the form of energy. The conversion rate of mass into energy is 4.26 million metric tons a second. This type of reaction is what occurred in a hydrogen bomb. So just like the bomb, that explosion is what happens in the sun but not exactly. Because the sun is so dense with hydrogen and helium, the explosion is contained. The outer mantle of the sun, which makes up three fourths of the sun and consists of all of the energy that is created by the core, contains this explosion. Plus the inward gravitation pull on itself also keeps the explosions contained.

The supernova is the explosion of a star and is one of the largest explosions in the universe. A supernova can outshine an entire galaxy for days or even months depending on the size. A supernova is formed when there is a change in the core of the star. This can occur in two ways. The first way happens when two stars orbit the same point and steal mass from each other and the star eventually becomes large enough that it will explode causing a supernova. The second way occurs when a star reaches the end of its lifetime and runs out of fuel, some of its mass will flow to the center of the star making heavier and eventually becoming so heavy it collapses in on itself and causes a supernova. Supernovas are very helpful in telling scientists about our universe. One way is that one supernova has shown that our universe is expanding at an increasing rate. Supernovas are also responsible for distributing many elements. Most of the atoms in our universe are actually manufactured inside a star. Stars have the ability to distribute elements up to iron, but to get heavier elements such as mercury, there would have to be a

Nuclear fusion is an atomic reaction where atoms combine to form a bigger atom with less mass. The most common nuclear fusion is when hydrogen nuclei forms helium nuclei. This occurs in stars that are small such as our sun. When there is low amount in nuclear fuel a star then turns into a red giant as its core grows smaller, denser, and hotter. Our sun will eventually turn into a red giant, theoretically vaporizing Earth. Once the core has nothing to fuse but iron, it will immediately begin the final phase. The temperature in the core rises over 100 billion degrees and then the star explodes. After a supernova, all that’s left of the star is a small, dense core called a neutron star. Also after the explosion, a black hole

Catastrophic explosion that ejects most of its mass is the reason the star suddenly increases greatly in brightness. The changes in the core of the star is when a Supernova is formed. A change that happens in two ways, both equal 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.

The longevity of a star’s life depends highly on its mass. Bigger stars burn through hydrogen more quickly, using up their fuel in a shorter amount of time and smaller stars burn through their fuel more more slowly, lasting longer, and therefore surviving for sometimes trillions of years. After the core runs out of hydrogen to burn, the fusion inside this “gigantic hydrogen bomb” slows down and begins to move to the outer layers of the star, heating up the surface, causing the star to expand, creating a red giant. During this time, the unstable, collapsing core heats up and begins fusing the helium atoms into carbon and carbon into oxygen, continuing the process and producing heavier elements and releasing more energy.After the core runs out of this fuel, there is no energy to fight against gravity and it collapses into a dense white dwarf, cooling over billions of years and eventually falling apart. Larger stars, however, undergo a different demise. These stars become massive red giants referred to as supergiants, producing carbon until “carbon builds up so much that their core collapses under the weight” (DK). The extreme heat produced by the allows supergiants to continue the fusion process with heavier elements, such as magnesium, sulfur, and silicon until they produce iron, an element that is lethal to the biggest of stars.