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The Life of a Star

This is a description of the life cycle of a star. One is an average sized star and the other is a star 10 x the Sun.
by

Wanita Telusnord

on 19 May 2012

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Transcript of The Life of a Star

The Life of a Star By Wanita Telusnord Nebula Main Sequence Stars Massive Protostar Massive Main Sequence Protostars Super Gaints Super Nova Neutron Star Black Hole Average Size Star Ten Times the size of the Sun Cloud of gas (hydrogen) and dust Birthplace of Stars Different types of Nebula Emission Nebula Glows Brightly Gas in it is energized by thye stars that have formed within it Reflection Nebula Starlight Grains of Dust Dark Nebula Dense clouds of molecular Absorb the light from stars Planetary Nebula Outer layers of stars that are lost Changes from a red giant to a white dwarf Temperatures exceed 20,000 K Surrounds a young star cluster Different energy levels Formed when old stars of a particular size, similar to our Sun's size, have consumed most of their hydrogen fuel after billions of years Hydrogen has mostly been converted to helium Expands to become a Red Giant Spectacular objects Extremely difficult object to view Clouds of gas and dust that absorbs some light from behind them.The light that is absorbed heats up the dust particles. Red Giant White Dwarf Twilight Darkness Different Shapes Size Hot Cold Warm Blue Red Elements Massive Born Life Death Light Years Magnitude Dense Masses Gravity Heat Red Dwarf Very cool Faint Small 1/10th the mass of the Sun Burns extremely slowly 100 billion years estimated to live Nuclear energy supplies have been used up Shrunken remains of Normal Stars Small, Hot Star Last stage in the life cycle Mass similar to that of the Sun 1% of the Sun's diameter approximately the diameter of the Earth 8000C or more overall luminosity's are 1% of the Sun or less They consume their stores of hydrogen fuel at a fraction of the rate that a star like the Sun. The largest known red dwarf has only 10% the luminosity of the Sun. Generate as little as 1/10,000th the energy of the Sun Large Bight Stars Cool Surface Hydrogen fuel at its center Converts hydrogen into helium in their core which is known as nuclear fusion. Expand many times its original size Diameter's between 10 and 100 times that of the Sun 2000-3000C Composed mainly of neutrons Produced when a supernova explodes Protons and Electrons combine to produce a Neutron Star Very Dense Diameter of only 20KM Belived to spin very rapidly Average ones have the mass of three times the Sun Formed from massive stars Gravitational pull Nothing can escape from it Suck in neighboring surrondings including nearby stars Light can not even escape the force Distort the space around them The Density of matter can not be measured Absorbs the light that hit the horizon Exsplosive death of a star Two Types: Type One: Type Two: Binary star systems Gas from one star drops on to a White Drawf, and then it explodes Stars ten times or more as massive as the Sun Suffer runaway internal nuclear reactions Leave behind neutron stars and black holes Thought to be main source of elements heavier than hydrogen and helium due to te fact they explode so strongly Formed when a star runs out of hydrogen fuel in their core Stars with more than about 10 solar masses, when after burning their hydrogen they become red supergiants during their helium-burning phase. Radius between 200-800 that of the Sun The most Massive Stars Supergiants can have masses from 10 to 70 solar masses Brightness from 30,000 up to hundreds of thousands times the solar luminosity Lifespans of only 10 to 50 million years They vary greatly in radii, usually from 30 to 500, or even in excess of 1000 solar radii Characterised by the source of their energy All undergoing fusion of hydrogen into helium within their cores Unchanging for long periods of time Explosion is as bright as 1 billion Stars 3 times bigger than the Sun Lifespand from 100,000 to 10 million Years Evolution of a young star Surrounded by a dense cocoon of gas and dust Blocks visible light Compacted Balls of Dust and Gas Large amounts of far infrared and microwave radiation From a interstellar gas cloud Composed primarily of hydrogen (97%) and helium (3%) Numerous reactions occur within the mass of forming star Majority of their lives Contracts over billions of years Pressure at the core continue to increase Temperature at the center of the star slowly rises over time Determind by there mass Shining Steadily 25% less bright than the present Sun OR Outer gaseous shell Core serves as the gravitational “center” of the star Very hot Very Dense Outer shell is made of hydrogen and helium gas Shell helps move heat Heat is released into space Blue Main Sequence Hydrogen fuses to form helium Much bigger in its expanding stage 90% of all stars Outer layer Expands
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