Star Life Cycle

After a time, the hydrogen runs out almost completely, and it collapses. New reactions begin to take place in the core and these reactions cause the star to expand rapidly. As the stars begin to deplete their new fuel, they switch to others. New elements are formed in the cores of stars but they become too heavy. The star has reached its end growth. When it reaches the end, a tremendous amount of energy is released and it begins to shed its outer layers, the gravity is too weak hold onto them anymore. Once the layers are removed, in the stars place is a fiery core called a planetary nebula. Eventually, the core runs out of fuel and it collapses. This star is now in a very dense state, and is called a white dwarf. Eventually, the white dwarf cools until it no longer shines. This dead star is called a brown dwarf.More massive stars, however, have more violent ways of dying. Some stars turn it into a supergiant. Supergiant stars are extremely bright, and are extremely large. Supergiant stars cores, can collapse violently and suddenly. This collapse causes a tremendous explosion, called a

The main idea for paragraphs 6-8 in When Stars Explode is how stars do explode. Here are some details: according to the text,“But these nuclear reactions do not make as much energy as hydrogen did. Within a few million years, the star has nothing left." The text also said “So the star's center collapses, scrunching itself into a small, dense object. Meanwhile, the star's outer layer shoots into space at millions of miles per hour. The star has exploded!"

The amount of fuel and the rate at which nuclear fusion occurs depends on the mass of the star. The mass of a star is the determining factor of how long it lives. A red-dwarf star is a star about half the size of our Sun. Due to its extremely low fusion rate, it is estimated that they could last for 10 trillion years. A medium-sized star like our Sun spends its main sequence stage up to 10 billion years.

A white dwarf is the leftover core of a planetary nebula. A white dwarf is a low-mass star that is virtually dead. Since it is a leftover core it is extremely dense. Inside of a white dwarf, no fusion takes place. The white dwarf will continue to give off light for about 20 million years and is theorized that it will then become a black dwarf. As of now, no black dwarfs have been discovered, simply because the universe is too young. A black dwarf gives off no light and is also cold, compared to the other stars in their life cycles. These black and white dwarfs burn through their fuel very slowly, which would be why they last for millions of

At some point in the future when the hydrogen runs out, at that point the star will start to collapse itself under its own weight. It get denser, hotter until the point where it starts to use the helium atoms themselves as the fuel for the fusion. As the star begins to fuse helium, it creates more energy and that causes the outer layers of the star to start to expand. One day our sun will grow so large that it will swallow up the inner planets of our solar system. It will become a red giant, for the sun this will be the beginning of the end. Then they explode and become a supernova or for some biggggggggggeeeeerrr stars it would be a hypernova, which is waaaayyy stronger than a supernova; supernovas are some of the most beautiful sights in the universe. Lucky for us, our sun is too small to even explode and become a supernova. These explosion of stars are so powerful that it can outshine the whole galaxy during its explosion. For the

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

Stage 10 in the death of a star, you would start to think that with the core collapsing, that the star would just collapse and break apart. However, this only happens with starts under ¼ Sol and takes about a hundred billion years at the least. However, a star like our Sun, doesn’t die quite that quickly. Even under all the collapsing and expanding as a Red Giant, the core starts to burn helium in its core. Once this burning is about 100 million Kelvin and the density in the core has risen to the right level, the helium begins to fuse with carbon, which causes the reactor in the centre of the star to

After approximately 10 billion years after the star is considered to be a main sequence star, the hydrogen at the center of the core is depleted. This causes the nuclear fusion which had been previously fueling the star to die out. Helium replaces the hydrogen in the core, and the inner core begins to shrink due to gravity. This process speeds up once all the hydrogen is completely used up. The radius of the star has increased

it runs out of energy. Once the star dies, it may become a white dwarf, a neutron star, or a black

One day the universe will turn dark forever as the last star fizzles out and that star will most likely be a red dwarf. When a red dwarf star forms it possesses important properties that give it the potential to host rocky planets similar to Earth. Therefore the creation and resulting properties of red dwarfs form stars that can provide energy to planets which may one day be hospitable to life forms. First the process of formation of red dwarfs will be explained. Then, the properties of these stars will be examined. Finally, the importance of red dwarf stars’ existence will be considered.

The process of a dying star is a more complicated and time-consuming procedure (it would take a few billion years). In fact, the dying process of a star that is similar to our Sun is slightly different from a star that is more massive than our Sun. For a star that is similar to our Sun, the process began with it shrinking as it cooled down after it ran of hydrogen, and eventually collapsed due to its weight. Once the core of a star began to contract, it would heat up, causing the outermost layer to expand. At this stage of the process, the star is now known as a red giant. Afterwards, the core would be so hot that it began fusing helium into carbon. Once the helium ran out, the core would expand then cool down. Again, the upper layers would expand and formed a planetary nebula. Finally, the core cooled down and became a white dwarf, which it eventually became a black

It is a large bright star with a cool surface. Just like the Sun, it eventually runs out of hydrogen fuel at its center. Red Giants have a diameter of about 10 to 100 times the size of the Sun. The reason for why the Red Giants are so bright is because of its size, although there surface temperature is less hot than the Sun’s. If you were to measure the temperature, it would be about 2000 to 3000oC. Red Giants, very large stars, are also often called SuperGiants. These stars sometimes have diameter of up to 1000 times the size of the Sun, also having more than 1 000 000 times the luminosities of the Sun (Life cycle). These stars live for only a few thousand years to 1 billion years. Eventually the helium in the core runs out and fusion stops. The star shrinks until a new helium shell reaches the

A red giant star becomes a white dwarf star when it runs completely out of hydrogen fuel in its core and it lacks the mass to force higher elements into fusion reaction. “The outward light pressure from the fusion reaction stops and the star collapses inward under its own gravity”. (www.universetoday.com) A white dwarf was a very hot star once, so therefore it shines. A white dwarf star will cool down until it becomes part of the background temperature of the universe. The process takes hundreds of billions of years.

Then, overtime the giants gasses drift away from the core then the gasses appear as a cloud around a dying sunlike star. When the clouds disperse, gravity causes the remaining matter in the core to collapse inward. The core becomes denser and very hot, then the star becomes a white dwarf. A white dwarf is the hot, dense core of matter that remains from the collapse of a low mass

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.