Omega Centauri: The Origin Of Globular Clusters

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

So many scientists have tried seeing this star close up and trying to find out if humans can be able to live there.And there are a lot more things that they still need to know about this star and how it got their.Scientists have known about this star for a very long time but still not confirmed if it is safe to go there.This star is the only star that is the closest the sun and not that far from the earth.So that is what i know about the star Proxima centauri and what they have discovered about this star that they call the earth-like

Let 's start with a Globular cluster, this is a well-shaped well-rounded cluster that consists of one very bright and dense star That gets surrounded by many smaller stars that were pulled in by its great gravitational pull. As explained in the last paragraph an open cluster is when a star blows through a nebula causing the stars and dust to separate but still didn’t fully fall out of its gravitational pull. Emission nebula are one of the most common nebulas that are seen. This Nebula is emitted by a hot star that releases photons which is a quantum of light. A reflection nebulae is that nothing but an actual cloud of dust

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 life cycle of a star is dependent on its mass. The larger the mass, the quicker it will die out, whereas stars which are no more than half the size of our Sun can live up to hundreds of billion years. However no matter how large the star is, they all begin their lives in a nursery known as a molecular cloud.

The amazing amount of radiation coming from the disk of gas is ripping the galaxy apart.

The Low mass stars spend there main life as a fusion machine which turns hydrogen into helium and a very slow and methodical pace. When the energy released by this fusion reaches the surface it is released into space and this is the star luminosity. Over a long, long time sometimes billions of years a low mass star consumes the hydrogen in its core and converts it to helium, at which point the core starts to contract and shrink. Once all of the hydrogen inside the stars core begins to become totally exhausted, the core pressure gives way to the crush of gravity because it has no more fusion occurring in its core at that time. As the core shrinks rapidly and the outer layers start to expand the stars shape begins to grow in size and its luminosity becomes extraordinary brighter due to the outer shell starting to produce fusion more rapidly then the core did during the main sequence life of the star. As this situation grows more rapidly and extreme the core starts to rapidly burn again and fuse its core helium into carbon. Then just before its final death the star ejects its outer layers into space. This leaves only the degenerate carbon core and since this core is still very hot it emits intensely powerful ultraviolet radiation and glows brightly in what is known as a planetary nebula. The nebula fades and cools over around a million or so years and we are left with a white dwarf cooling indefinitely till

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

I can tell many things about the star B-Centauri by looking at this H-R diagram. First of all I can see that it has a temperature of almost 30,000 K, that means it is almost five times hotter than our sun. Next, B-Centauri's luminosity is 10, 000 Lu which means it produces ten thousand times the energy of our sun. I know that B-Centauri is a spectral type O by reading the H-R diagram. During the Vlab we found that Naos was a spectral type O. All stars that are spectral type O are blue, meaning they are the hottest type of stars. Stars of the same spectral type have the same composition. Since Naos has hydrogen, helium, and helium ions so does B-Centauri. The mass of B-Centauri is twenty times the mass of our sun. The radius of B-Centauri

I can tell many things about the star B-Centauri by looking at this H-R diagram. First of all I can see that it has a temperature of almost 30,000 K, that means it is almost five times hotter than our sun. Next, B-Centauri's luminosity is 10, 000 Lu which means it produces ten thousand times the energy of our sun. I know that B-Centauri is a spectral type O by reading the H-R diagram. During the Vlab we found that Naos was a spectral type O. All stars that are spectral type O are blue, meaning they are the hottest type of stars. Stars of the same spectral type have the same composition. Since Naos has hydrogen, helium, and helium ions so does B-Centauri. The mass of B-Centauri is twenty times the mass of our sun. The radius of B-Centauri

In this stage, it spent time to fuse from hydrogen to helium in the core of star. When hydrogen starts to run out, the core starts to contract and becomes unstable. The outer shell starts to cool down and turns red since the outer shell is mostly hydrogen. The Sun is the main sequence and the stars in the main sequence can be classified into spectral types with each class. Each spectral type are divided into several sub-division such as A0 being the most hottest stars and A9 being the least hottest stars of group A. Similarly, M, K, G, F, A, B and O spectral classes are used to classify each star. G-type star is the Sun, which is the main sequence. O type is the most complex molecule observed in the interstellar medium. M spectral type is the most abundant in our galaxy. As, the stars were arranged by color from blue-white to red that is spectral type B through M. The arrangement was also performed in luminosity where hottest stars were more luminous than the cooler stars. The hottest stars are blue in color that is very rare and coolest star are red in color that is

As they develop, bars apparently become one of the most important catalysts for galaxy evolution. They force a large amount of gas towards the galactic center, fueling new star formation, building central bulges of stars, and feeding massive black holes. Galaxies are thought to initially assemble from, and grow in size through, mergers with other smaller galaxies. After this phase is complete, however, the only other dramatic way for galaxies to evolve is through the action of

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

In lab six our topic was a continued learning about the Herstsprung-Russell diagram. We will discuss the properties needed to plot an open cluster of stars called the Pleiades cluster. Using the HR diagram we identified the temperature, age and characteristics of these main sequence stars. We applied all of this data and plotted it on our own diagram. From there we answered questions about different results that were found.

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.