'Science of Stars\r'

'Stars be swell up recognized astronomical objects in our solar dodge and represent building blocks of galaxies. The history and dynamics of a star in a galaxy depends on its age, distribution, and composition. The stars ar responsible for elements such as carbon, nitrogen, and oxygen. A star’s life begins very small, akin mevery more things in the universe. They begin as, as below from anything else, particles in clouds of dust and foul up. They re master(prenominal) cold for ages. The incumbrance of a comet or other object that hunts with the cloud forget indeed make particles bump around and clumps will begin to form.\r\nOver the course of a million years, clumps will grow into what we call â€Å"protostar” and transcend in more gases and grow even hotter. This is how stars be formed and is a point in a star’s life. Astronomers determine composition, commentise, and temperature of stars and other nonadjacent objects with an essential tool ca lled a spectroscopy. Astronomers acquit employ this tool since the 1800’s to analyze emitted light spectra. When a star gives off light and the light splits by prism, the spectral pattern reflects a star’s composition. All stars atomic number 18 95% hydrogen, so the variations in composition reveal its age, luminosity, and origin.\r\nComposition of gases advise be determined by observing the light of a star. Astronomers can determine the temperature of a star from its color and its spectrum. All stars maintain antithetic colors. They have different colors due to its light radiation. There atomic number 18 a few different ways astronomers can determine a star’s temperature. single way is to measure a star’s color. They use three filters that transmit light in three different wavelength ranges. Astronomers then take the gaudiness ratio of the light. Another way to determine the temperature of a star is to examine the spectral lines in the starligh t.\r\n accomplishment of Stars3 Astronomers withal use a tool called the electromagnetic spectrum to determine the composition, temperature, speed, and revolution rate of stars and other opposed objects. Rotation rates atomic number 18 measured by apply telescopes or space probes. Astronomers pick a particular feature on an object and then determine how long the feature takes to bear upon from angiotensin converting enzyme side to the other side. For an example, the sunlight has a rotation rate of well-nigh 25 days. One planet in our solar system that is difficult for astronomers to come rotation rate is mankind.\r\nThat is because we live on commonwealth and rotate with it. As stars progress through their lives they move around in the H-R diagram since their properties change oer a period of time. In the H-R diagram it plots luminosity, spectral type, and also temperature. If a star is plan high up on the diagram on the straight plane, this means that the stars are b righter. If a star is plotted in the horizontal plane to the left wing, this means that these stars are the hottest. Stars drop down most of their lifetime in what is cognise as the main epoch in the H-R diagram.\r\nIn this descriptor of a star’s life, they enkindle hydrogen into helium. Also at this point, the star’s size and luminosity remain constant because their forces have reached a near-equilibrium. Stars will remain in the main epoch until they reach a certain vision. Stars that are called supergiants in the H-R diagram and lie along the pourboire right are bright and cool. The stars that are called washcloth dwarfs and are plotted at the bottom left of the diagram are fainter, hotter stars. The red giant stars are the stars of great luminosity and size. They form a heavy horizontal band that joins the main sequence.\r\nAll the stars on the H-R diagram are plotted by their color horizontally and their luminosity vertically. All the colors are code d from O (blue), B (blue), A (blue-white), F (white), G (yellow), K (orange), and M (red). erudition of Stars4 In the focalise of our solar system lies a star called â€Å"the lie”. Its color is white, but appears to us on Earth as yellow and is considered a main sequence star. The life cycle of the fair weather, just like any other star starts with a cloud of gas and dust composed mainly of hydrogen collapses under gravitational forces.\r\nIt was formed about 4. 5 one million million million years ago determined by scientists using the temperateness’s current main sequence age. Right now, the Sun is believed to be about middle(a) through its main sequence evolution. The Sun should spend about 10 one thousand thousand years as a main sequence star. It will tangle with the red giant set up in about 5 billion years. By the time it reaches to be a giant star stage, the Sun will have lost about 30% of its mass due to a stellar wind. The orbits of the planets will move outward then. Eventually our Earth will be swallowed by the Sun.\r\nThe Sun living in the main sequence is gradually becoming more luminous and its temperature is slowly rising. After the red giant stage, the Sun’s outer layers will be impel off. It will cool and fade into the white dwarf stage. As of right now, the Sun’s life cycle is the main sequence stage. It is considered middle old at 4. 5 billion years old. The Sun is currently fusing hydrogen in its core and has been for the snuff it 5,000 million years, and it is expected to continue fusing hydrogen for at least another 4,000 million years.\r\nThe main sequence stage is the longest and most stable phase of its existence and this stage lasts about 10 billion years for a star. The main sequence is also the first stage of a star afterwards becoming a star, right after the protostar stage. The quest stage after the main sequence stage would be the red giant stage. I have now discussed in this paper how astronomers determine composition, temperature, speed, and rotation rate of distant objects. I explained the properties of the stars in the H-R Science of Stars5 diagram, summarized the life cycle of the Sun, and also stated where the Sun is currently in its life cycle.\r\n'