Research Paper On Sequence Stars

In about 5 billion years, the Sun will become a red giant. A red giant is a star which has completely

Comparing red giants to the sun, they are about 1000 times larger. Compared to the sun’s temperature, a red giants temperature is about half as much. This is because the same amount of energy has to be spread out across a much more massive star causing it to be cooler than it was before. The name red giant was given to these stars because the change in temperature causes the star to shine in the redder part of the spectrum. Stars can spend anywhere between 1000 years and one billion years in the red giant phase. After a certain amount of time, the helium finally runs out and fusion stops. Since there is no more helium, gravity pushes the star inward. The stars outer atmosphere is then blown out into huge clouds of gas and dust which is known as planetary nebulae. These clouds of gas and dust are then made to make new stars. As for the core of the star, it is still there. The star is now a white dwarf. White dwarf stars occur when the red giant loses its outer atmosphere. White dwarf stars are extremely hot because they are composed of only the core of the star which is the hottest

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.

Planetary nebula are formed in the outer core of the star that are vanished when the star of the Sun’s mass changes from a red giant to white dwarf. At this stage all the energy from the star fades away losing layers and forms a complex structure.

When a sun like star like the sun sheds most of it’s mass it is called a planetary nebula.

A Solar Mass Main Sequence Star will stay in its newborn state for about 90% of its life however when it is time to return to the universe, it must go through many stages before its final curtain call.

By running out of fuel the star is no longer able to oppose gravity and keep itself stable so it collapses on itself until it reaches a singularity. Once it becomes a black hole it can have a mass ranging from just a few times the mass of our sun to over a billion times. The gravity of a black hole varies with its size however the center of a black hole is considered a singularity due to its ability to have an enormous amount of mass in an infinitely small space. A black hole is seen as black due to its escape velocity being greater than the speed of light, because it is faster than light no light can escape therefore there is none for us to view making it appear black. An objects escape velocity is the speed required for an object to leave an objects field of

3. A smaller star has less fuel, but its rate of fusion is not as fast. Therefore, smaller stars live longer than larger stars because their rate of fuel consumption is not as rapid.

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 giant stars die in supernova and their core collapse that is when a neutron star is created.This neutron star is several times bigger than the sun.Because the neutrons are tightly put together into a super dense object the supernova is very heavy it weighs about 100 million tons.

The Nebula becomes a Protostar, the second stage of a star’s life cycle, once the ball of gas and dust starts to shrink because of it’s own mass and gravity. The Protostar is still not a star yet. At this stage it can be up to 100x larger than our Sun! The Protostar will keep shrinking and start to heat up, until it becomes roughly the size of our Sun.

Stars a balls of gas that are luminous meaning that they give off light. Star first start transition begins from clouds, a cold molecule of hydrogen that gravitationally collapse creating fragments into many pieces that slowly form in to individual stars. Stars are then held by their own gravity and is made of 75% hydrogen and 25% helium two of the elements in the periodic table. Hydrogen has the symbol of H and is the lightest and also simplest element in the periodic. Helium had the symbol He and had the lowest boiling point compared to the other elements in the periodic table. As time eclipse stars converts elements of hydrogen to helium that is why the ratio of the sum is 70% hydrogen and 29% helium.

White dwarf formed, particularly when there is availability of multiple stars; from this multiple star, it can experience similar exciting end as a nova. The gravity of this star may drag the hydrogen from the external layer of star onto itself because of the closeness with the other.

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

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.