Stars are hot because nuclear reactions happen inside them. Those reactions are called nuclear fusion. Nuclear fusion makes light and heat and makes bigger and bigger chemical elements. Stars have a lot of hydrogen. Nuclear fusion changes hydrogen into helium. When a star gets old, it starts to change the helium into other bigger chemical elements, like carbon and oxygen. Fusion makes a lot of energy. The energy makes the star very hot. The energy produced by stars moves (radiates) away from them. The energy leaves as light which we call electromagnetic radiation.
Earth's Sun[change | change source]
The star nearest to Earth is the Sun. The energy from the Sun supports almost all life on Earth by providing light for plants. Plants turn the light into energy in a process called photosynthesis. The energy from the Sun also causes weather on Earth.
We can see other stars in the night sky when the Sun goes down. Like the Sun, they are made mostly of hydrogen and a little bit of helium plus other elements. Astronomers often compare those other stars to the Sun. For example, their mass is given in solar masses. A small star may be 0.2 solar masses, a big one 4.0 solar masses.
Planets[change | change source]
The Earth and other planets move around (orbit) the Sun. The Sun and all things that orbit the Sun are called the Solar System. Many other stars have planets orbiting them: those planets are called exoplanets. If you were on an exoplanet, our Sun would look like a star in the sky, but you could not see the Earth because it would be too far away.
Numbers, distances[change | change source]
Astronomers think there are a very large number of stars in the Universe. They estimate (guess) that there are at least 70 sextillion stars. That is 70,000,000,000,000,000,000,000, which is over 200 billion times the few hundred billion stars in the Milky Way (our galaxy).
Most stars are very old. They are usually thought to be between 1 billion and 10 billion years old. The oldest stars are 13.7 billion years old. That is as old as the Universe. Some young stars are only a few million years old. Young stars are mostly brighter than old ones.
Stars are different sizes. The smallest stars are neutron stars, which are actually dead stars. They are no bigger than a city. The neutron star has a large amount of mass in a very small space.
Hypergiant stars are the largest stars in the Universe. They have a diameter over 1,500 times bigger than the Sun. If the Sun was a hypergiant star, it would reach out to as far as Jupiter. The star Betelgeuse is a red supergiant star. Although these stars are very large, they also have low density.
Some stars look brighter than other stars. This difference is measured in terms of apparent magnitude. There are two reasons why stars have different apparent magnitude. If a star is very close to us it will appear much brighter. This is just like a candle. A candle that is close to us appears brighter. The other reason a star can appear brighter is that it is hotter than another cooler star.
Stars are made of mass and mass makes gravity. Gravity makes planets orbit stars. This is why the Earth orbits the Sun. The gravity of two stars can make them go around each other. Stars that orbit each other are called binary stars. Scientists think there are many binary stars. There are even groups of three or more stars that orbit each other. Proxima Centauri is a small star that orbits other stars.
Stars are not spread evenly across all of space. They are grouped into galaxies. A galaxy contains hundreds of billions of stars.
History of seeing stars[change | change source]
Astronomers organized stars into groups called constellations. They used the constellations to help them see the motion of the planets and to guess the position of the Sun. The motion of the Sun and the stars was used to make calendars. The calendars were used by farmers to decide when to plant crops and when to harvest them.
The life of stars[change | change source]
Stars are made in nebulas. These are areas that have more gas than normal space. The gas in a nebula is pulled together by gravity. The Orion nebula is an example of a place where gas is coming together to form stars.
Stars spend most of their lives combining (fusing) hydrogen with hydrogen to make energy. When hydrogen is fused it makes helium and it makes a lot of energy. To fuse hydrogen into helium it must be very hot and the pressure must be very high. Fusion happens at the center of stars, called "the core".
The smallest stars (red dwarfs) fuse their hydrogen slowly and live for 100 billion years. Red dwarfs live longer than any other type of star. At the end of their lives, they become dimmer and dimmer. Red dwarfs do not explode.
When very heavy stars die, they explode. This explosion is called a supernova. When a supernova happens in a nebula, the explosion pushes the gas in the nebula together. This makes the gas in the nebula very thick (dense). Gravity and exploding stars both help to bring the gas together to make new stars in nebulas.
Most stars use up the hydrogen at their core. When they do, their core becomes smaller and becomes hotter. It becomes so hot it pushes away the outer part of the star. The outer part expands and it makes a red giant star. Astro-physicists think that in about 5 billion years, the Sun will be a red giant. Our Sun will be so large it will eat the Earth. After our Sun stops using hydrogen to make energy, it will use helium in its very hot core. It will be hotter than when it was fusing hydrogen. Heavy stars will also make elements heavier than helium. As a star makes heavier and heavier elements, it makes less and less energy. Iron is a heavy element made in heavy stars.
Our star is an average star. Average stars will push away their outer gases. The gas it pushes away makes a cloud called a planetary nebula. The core part of the star will remain. It will be a ball as big as the Earth and called a white dwarf. It will fade into a black dwarf over a very long time.
Later in large stars, heavier elements are made by fusion. Finally the star makes a supernova explosion. Most things happen in the universe so slowly we do not notice. But supernova explosions happen in only 100 seconds. When a supernova explodes its flash is as bright as a 100 billion stars. The dying star is so bright it can be seen during the day. Supernova means "new star" because people used to think it was the beginning of a new star. Today we know that a supernova is the death of an old star. The gas of the star is pushed away by the explosion. It forms a giant cloud of gas called a planetary nebula. The crab nebula is a good example. All that remains is a neutron star. If the star was very heavy, the star will make a black hole. Gravity in a black hole is extremely strong. It is so strong that even light cannot escape from a black hole.
The heaviest elements are made in the explosion of a supernova. After billions of years of floating in space, the gas and dust come together to make new stars and new planets. Much of the gas and dust in space comes from supernovae. Our Sun, the Earth, and all living things are made from star dust.
Colors[change | change source]
Astronomers have known for centuries that stars have different colors. When looking at an electromagnetic spectrum, ultraviolet waves are the shortest, and infrared are the longest. The visible spectrum has wavelengths between these two extremes.
Modern instruments can measure very precisely the color of a star. This allows astronomers to determine that star's temperature, because a hotter star's black-body radiation has shorter wavelengths. The hottest stars are blue and violet, then white, then yellow, and the coolest are red. Knowing the color and absolute magnitude, astronomers can place the star on the Hertzsprung-Russell diagram, and estimate its habitable zone and other facts about it.
For example, our Sun is white, and the Earth is the perfect distance away for life. If our Sun was a hotter, blue star, however, Earth would have to be much farther away or else it would be too hot to have water and sustain life.
References[change | change source]
- Simon A. 2001. The real science behind the X-Files: microbes, meteorites, and mutants. Simon & Schuster. pp. 25–27. ISBN 0684856182. http://books.google.com/?id=1gXImRmz7u8C&pg=PA26&dq=bacteria+that+live+with+out+the+sun.
- Forbes, George (1909) (Free e-book from Project Gutenberg). History of Astronomy. London: Watts & Co.. ISBN 1153627744. http://www.gutenberg.org/etext/8172.
- Hevelius, Johannis (1690). Firmamentum Sobiescianum, sive Uranographia. Gdansk.
- Tøndering, Claus. "Other ancient calendars". WebExhibits. http://webexhibits.org/calendars/calendar-ancient.html. Retrieved 2006-12-10.
- "The Electromagnetic Spectrum". Andy Darvill's Science Site. http://www.darvill.clara.net/emag/. Retrieved 6/6/2016.
- "Star Colors Explained". One Minute Astronomer. December 23, 2008. http://oneminuteastronomer.com/708/star-colors-explained/. Retrieved 6/6/2016.
Related websites[change | change source]
|The Simple English Wiktionary has a definition for: star.|
- Media related to Star at Wikimedia Commons
- Green, Paul J (2005). "Star". World Book Online Reference Center. World Book, Inc. http://www.nasa.gov/worldbook/star_worldbook.html. Retrieved 2010-08-20.
- Kaler, James. "Portraits of Stars and their Constellations". University of Illinois. http://www.astro.uiuc.edu/~kaler/sow/sow.html. Retrieved 2010-08-20.
- "Query star by identifier, coordinates or reference code". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/sim-fid.pl. Retrieved 2010-08-20.
- "How To Decipher Classification Codes". Astronomical Society of South Australia. http://www.assa.org.au/sig/variables/classifications.asp. Retrieved 2010-08-20.
- "Live Star Chart". Dobsonian Telescope Community. http://www.mydob.co.uk/community_star.php. Retrieved 2010-08-20. View the stars above your location
- Prialnick, Dina; Wood, Kenneth; Bjorkman, Jon; Whitney, Barbara; Wolff, Michael; Gray, David; Mihalas, Dimitri (2001). "Stars: Stellar Atmospheres, Structure, & Evolution". University of St. Andrews. http://www-star.st-and.ac.uk/~kw25/teaching/stars/stars.html. Retrieved 2010-08-20.