Red Dwarfs 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

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

In this paper I will explain how astronomers determine the composition, temperature, speed, and rotation rate of distant objects using various methods. I will explain the properties of stars. I will also summarize the complete lifecycle of the Sun and determine where the Sun is currently in its lifecycle.

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.

Red giants are dying stars that are in their last part of stellar evolution. Every star will eventually turn into a red giant over some point in time. Stars turn into red giants when there is no more hydrogen fuel for the star. Inside of a star, hydrogen goes through a process called nuclear fusion where hydrogen is getting converted into helium. Nuclear fusion helps create energy for the star so that the force of gravity isn’t crushing the star together. This is also the reason why stars are bright. When the star runs out of hydrogen to convert into helium, the energy that kept the star from collapsing is now gone. Gravity then takes over and compresses the star. From this point, the helium atoms are able to combine

A red dwarf star is considered to be a great spot for life because of its potential for long term habitability. For earth, the habitable zone it resides in lasts only about 7 to 10 billion years. Compare that to a red dwarf, where a habitable zone can last for for a span almost five times greater than that for earth. Thus making a red dwarf a good candidate for life to grow, develop and become advanced. Another point to consider is that many planets orbiting M dwarf, red dwarf stars are highly likely to have large amounts of water which suggests the idea that there could be many habitable planets surrounding a red dwarf star. However, red dwarf stars have a few big problems. Due to the low luminosity of a red dwarf, planets have to be relatively close for it to be in the known habitable zone. And by being so close, planets face hostile conditions. One condition is the barrage of stellar wind, which could strip a planets atmosphere. Another is that the planet could be tidally locked, so only one side would face the star. Lastly, is that red dwarf stars are emit extreme EUV and X ray

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

White dwarf is very small with diameter as the Earth and mass similar to the Sun formed when the core of red giant collapsed. The maximum mass a white dwarf can have is about 1.4 solar masses which is known as Chandrasekhar limit. A single star can be one mass at the start of life and still evolve into a white dwarf being 0.6 mass compressed into approximately the volume of the Earth. Even though it is hot, it is not as bright compared to its temperature of more than 8000° C. However, they cool down and fade over billions of years.

This article discusses a new planet that could end up supporting life. This new planet is called Proxima b because it orbits a star called Proxima Centauri. Proxima Centauri is a red dwarf star. Red dwarfs are composed of “a cloud of dust and gas that is drawn together by gravity and begins rotating.” (Reed, 2016) They are called dwarfs because they only weigh “7.5 to 50 percent of the mass of the sun.” (Reed, 2016) Since these stars are small, they only reach up to 6,380 degrees Fahrenheit. Red dwarf stars can last trillions of years. “Their limited light and heat meant that the habitable zone-the region where liquid water could form, and thus life would be considered most likely to evolve.” (Reed, 2016) Proxima Centauri is an example of

This causes the ball, now a star, to shine. Depending on the mass of the star, they can reach different types of fusion. Normal stars that have a mass of up to 4 times the sun can only have hydrogen fusion, helium fusion, and carbon fission. Stars with a bigger mass is classified as a massive star, and they undergo multiple stages. They start out similar to the normal stars with hydrogen fusion, helium fusion and carbon fission, but continue over to oxygen fusion, and silicon fusion. The end product of Silicon is Iron. No star can fuse Iron, it will die. How much gas and dust is collected during the star’s formation determines the size and colour of the star. As time passes by, stars fight the inward pull of the force of gravity. The outward pressure created by the nuclear reactions pushing away from the star's core keeps the star whole. However, these nuclear reactions require hydrogen. Eventually the supply of hydrogen in the core runs out and the star begins to

Most stars, around 70 percent, are red dwarves, which are less massive than the sun. These stars are immortal, to our purposes. Their lives are several orders of magnitude longer than the sun's. There are many more that aren't red dwarves but are still less massive than the sun. Most stars we can see with the naked eye, however, are more massive, and stellar lifetime decreases rapidly with mass. There isn't a red dwarf close enough to be seen naked eye. So most that you see in the

At that point, the star begins to fuse helium into carbon in the core. This is called helium fusion. In order for this to happen, the core’s density has to increase and the temperature has to reach about 100 million Kelvin. However, a complication arises when helium fusion begins. The star’s core is degenerated and the burning becomes unstable since the core is not able to accommodate the fusion. The increase of internal pressure and temperature caused by the burning of the helium leads to an astronomical increase in outward pressure. This is, eventually, able to regulate and the core is able to expand and decrease its

(2) Sub-stellar objects with true masses above the limiting mass for thermonuclear fusion of deuterium are brown dwarfs, no matter how they formed nor where they are

This would mean that the theory that dwarfs form similarly to stars despite being smaller and such holds true. If dwarfs had not emitted jets or done anything like this, it would mean that the dwarfs have a similar formation to that of planets.

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.