Termar Neebula Made Out Of Stars Essay

Star formation is a rather simple process. Gasses in space clump together with dust and rock. Over millions of years these materials begin to form small orbs. Eventually it the clump will get big enough to create gravity. The core will become hot from the constant pressure and will use hydrogen to make helium using nuclear fusion. This fusions creates a tremendous amount of energy creating a fiery ball in space.

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

Thesis Statement: Supernovas are big explosions of light that occur when a star has a lot of fuel inside it which causes the star to explode.

Stars like our Sun, which are no more than 1.44 solar masses, will undergo fusion of hydrogen into helium. Over its life time the star slowly uses its supply of hydrogen by fusing it into helium. These reactions require high temperatures. Eventually the star will completely fuse hydrogen into helium in its core leaving inadequate amounts of thermal pressure to balance gravity. This will cause the centre of the star to contract to compensate for the heat energy lost.

Stage 8 is when the star starts to run out of fuel. It has spent close to 10 billion years burning hydrogen in its core and now it’s starting to run low and almost empty of the fuel it requires to keep burning. As the hydrogen starts to run low, helium levels start to increase in the higher temperature core as well as on the surface. However, the surface helium isn’t as noticeable because it doesn’t burn as high or fast as the inner core. But as the hydrogen completely runs out, the nuclear fusion subsides and a core of non-burning helium grows, forcing the burning of the star to head out of the inner core and up to the outer core. At this point, the radius of the star starts to grow rapidly because of the gas pressure and the core shrinks under the pressure of gravity.

The burning process continues in the outer layers of the star, and they continue to expand. They can reach a maximum radius of approximately 300 times our Sun’s! The burning in the outer layers becomes unstable and they go through a series of explosive helium-shell flashes which are brought on by the pressure in the shell and the sensitivity to changes in temperature. This process causes the outer layers to pulse as they heat and expand, and then cool and contract. The core contracts and heats up as the last of its fuel is used. It becomes so hot that it expels ultraviolet radiation into the inner parts of the surrounding cloud, ionizing it. This process is called a planetary

When we think of stars, we often think that they are all the same. We often think that they are all just big balls of gas burning up to billions of light years away. However, that isn't exactly true. The truth is that stars are very diverse. Just like anything else in our Universe, stars fall into many different classifications based on its defining characteristics. In this essay I will discuss several different types of stars.

Stage Eight: Nuclear fusion continues and as the hydrogen fuel is used up, the composition of the star's interior/core changes. At the center, the star's helium content begins to rise. Helium contents also rise at the edge of the core but it happens at a much slower rate. This is because the inner core's temperatures/burning rates are higher than the edge of the core. The inner core becomes bigger and bigger. After ten million years, the hydrogen is all gone from the center! The nuclear fire begins to slow and stop! Non-burning helium is now increasing in the core but outward pressure decreases. The structure of this star begins to change as the pull of gravity towards it does not decrease. The inner core shrinks and once the hydrogen is all

Type I supernova: star accumulates matter from a nearby neighbour until a runaway nuclear reaction ignites.

The colors of violet, rose, blue, orange, mint green, yellow and many more, make it look like a painting. This nebula with a giant star at its center is known as SBW2007, located in the Carina Nebula. A supernova burns for only a short period of time, but it can tell scientists a lot about the universe. One kind of supernova has shown scientists that we live in an expanding universe, one that is growing at an ever increasing rate. Scientists also have determined that supernovae play a key role in distributing elements throughout the universe. When the star explodes, it shoots elements and debris into space. Many of the elements we find here on Earth are made in the core of stars. These elements travel on to form new stars, planets and everything else in the

The inner core has reached its final high density state and the nuclear burning surrounding it increases in intensity. The helium burning becomes unstable and the shell becomes sensitive to changes in temperature and high in pressure, causing explosive flashes. The star’s outermost layers begin to expand and contract as they heat and cool in response to the flashes. Once the star exhausts the remaining fuel at its core, ultraviolet radiation ionizes the surrounding cloud and the star. The result is a planetary nebula, which is a round or oval shape created by the escaping of expanding

Stars spend approximately eighty percent of their lives on the main sequence before evolving into something else. A star leaves the Main Sequence when it has exhausted most of the hydrogen in its core, which causes it to lose equilibrium. It begins to contract again as radiation and thermal pressure decrease, and gravity dominates. Even though core hydrogen fusion ceases, energy is still generated in the core because of gravitational contraction. While the Main Sequence is the hydrogen core fusion stage, the first stage after the Main Sequence is the hydrogen shell fusion stage of a star’s life. During the hydrogen shell fusion stage, the nuclear fusion rate is considerably greater than during the Main Sequence. Changes in the outer layers of a star occur as the internal changes are happening. Increased pressure causes enormous expansion in the outer layers of the star, which leads to them cooling because they are farther away from the core. Visible

A star’s life cycle is determined by mass; the larger a star is, the shorter its lifespan is. When stars are formed, they begin as clouds of gas and dust in nebulae. Because of gravity, the matter condenses into a sphere where hydrogen is combined with helium, forming a protostar. As energy is released through nuclear fusion, stars enter the main sequence, the longest phase of a star’s life where it reaches stable nuclear reactions.

Since we first gazed upon the heavens, man has been perplexed over where the bright lights in the sky have come from. This report will provide information for the birth and death of both low and high mass stars that is supported by scientifically proven statements and observations. It is the long held belief of many, that molecular clouds are the nurseries of stars. These dense clouds of gas are most often found in the spiral arms of galaxies. Obviously, smaller cloud produce low mass stars while large clouds produce high mass stars which collapse much faster than their smaller siblings during the protostar phase ( Washington). At this point, the cloud is cool with very low pressure. Once these clouds of gas become dense enough, they collapse to create the beginnings of a star know

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.