Science of Stars Paper

I pick the star Antares, from the H-R diagram I can tell that it it is a Red Supergiant, and it has a surface temperature that is around 3,000 degrees kelvin, which is cooler than the Sun by at least 2,000 degrees kelvin, but its luminosity is around 10,000 solar units, which means it produces much more energy than our Sun does, so it is a lot brighter. The spectral type of Antares is a M, I could tell that its spectral type was M because I read the H-R Diagram, the VLab told me that the star ‘Betelgeuse’ has a spectral type of M, and Antares is right below, and basically inside Betelgeuse. Stars with the same spectral type have the same chemical composition, so Antares has the chemical composition Ca (calcium), TiO (titanium oxide), CH (methylidene).

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 sun is a big, hot ball of hydrogen gas which enables us to feel the sun’s heat and see its brightness. Every second of every day, the sun transforms over 700 million tons of hydrogen into over 600 million tons of helium. The sun produces so much energy that we can see the sun’s brightness and feel its heat. Hydrogen fusion takes place in the Sun’s core and the gas is heated by the energy that is discharged above the core. Ultimately the gas becomes less dense and the heat from below turns the gas

[27] Scientists can determine what a distant star is made of by looking at ____.

This lab was to inform us about the brightness of stars. We learned how to use the absolute magnitude and apparent magnitude to measure the luminosity of the stars. A stars brightness and magnitude are connected to each other. The lower numerical value of the magnitude the brighter the star will appear.

There are seven major spectral types. Stars range from blue and hot to red and cool. The spectral types are: O, B, A, F, G, K, and M (from hottest to coolest). Each of these letters is divided into 10 numerical classes, from hotter to cooler: 0, 1, 2, 3, 4, 5, 6, 7, 8, and 9. For example, our Sun has the spectral type G2. Spectroscopy is a scientific technique in which the visible light coming from objects (like stars and nebulae) is examined to determine the object's composition, temperature, density, and velocity. The spectrum is the band of colors that white light is composed of, in the order: red, orange, yellow, green, blue, indigo, violet (from long to short wavelength). Newton first discovered that sunlight could be divided into the visible spectrum. The compositions of stars are determined through spectroscopy. Spectroscopy is the study of something using spectra. Recall from the Electromagnetic Radiation chapter that a spectrum is what results when you spread starlight out into its individual

The stars are born from gas and dust. Even the sun formed this way. Stars are also classified by color, temp., luminosity, and distance from the earth. Stars form inside a cloud of dust called a Nebula. Gravity pulls gas and dust closer together in some place of the Nebula. When the matter contracts, it forms a hot sphere. Did you know the color of the star is the effect of the temperature of the star. The sphere then becomes a star if the center grows hot and dense enough for fusion to happen. As you can see stars, like the sun, are born out of gas and dust that gets contracted.The different stages a star goes through depends on the mass of the star. Lower-mass stars develop

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

A star has 5 definite stages and 3 stages which can vary between stars. The 5 definite stages are a Nebula, a Star, a Red Giant, a White Dwarf and a Red Dwarf. The stages that can vary are a Supernova, a Neutron Star and a Black hole. As the star goes through each stage, it can change size dramastically. An example of this is a Red Giant, which is 100 time the size of the Sun, compared to a Red dwarf, only 1 tenth the size of the sun (Life cycle). An interesting fact is “The closest star to Earth is Proxima Centauri, located 4.2 light-years away. In other words, it takes light itself more than 4 years to complete the journey from Earth. If you tried to hitch a ride on the fastest spacecraft ever launched from Earth, it would still take you more than 70 000 years to get there from here.” (Interesting facts)

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.

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

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.

This is the fourth stage of a star’s life cycle. The Star diameter will be about 700,000 km. An average star will live for about 10 billion years in this stage. Our Sun is only about 5 billion years old. After the Infrared becomes a Star, it will continue to burn changing more of its Hydrogen into Helium. Eventually the Hydrogen begins to run out, until the Star becomes a Red Giant.

The key features of stars which are of interest to astronomers are their mass, their luminosity, their surface temperature and the distance they are away from us.

Indecent bodies like the sun. Stars are made up of big exploding balls of gas, mostly hydrogen and helium. The sun is similarly a star made up of huge amounts of hydrogen, undergoing a continuous nuclear reaction like a hydrogen bomb. Stars come about when vast clouds of hydrogen, helium and dust contract and collapse due to gravity. The clouds came from astronomical plasma from “The Big Bang”, but the dust comes from the supernovae of other stars.