Sun - Revision history

Jmdonev: 1 revision imported

2021-09-27T00:02:50Z

1 revision imported

← Older revision	Revision as of 00:02, 27 September 2021
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energy>Luisa at 22:36, 9 September 2021

2021-09-09T22:36:09Z

← Older revision		Revision as of 22:36, 9 September 2021
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	[[Category:Done ~~2018~~-07-20]]		[[Category:Done 2021-01-31]]
			[[Category:Translated to French]]
			[[fr:soleil]]
			[[Category:Translated to Spanish]]
			[[es:Sol]]
	[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]		[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]
	<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about three quarters of its total [[mass]] - and [[helium]] - about one quarter of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>		<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about three quarters of its total [[mass]] - and [[helium]] - about one quarter of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>
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	==Layers of the Sun==		==Layers of the Sun==
	Satellites have been launched to study the Sun continually. These satellites observe the Sun in a variety of [[wavelength]]s that helps to create a picture that describes the inner workings of the Sun. The Sun is believed to be made up of 6 different regions:<ref>Tim Sharp. (July 31, 2015). ''Atmosphere of the Sun'' [Online]. Available: http://www.space.com/17160-sun-atmosphere.html</ref>		Satellites have been launched to study the Sun continually. These satellites observe the Sun in a variety of [[wavelength]]s that helps to create a picture that describes the inner workings of the Sun. The Sun is believed to be made up of 6 different regions:<ref>Tim Sharp. (July 31, 2015). ''Atmosphere of the Sun'' [Online]. Available: http://www.space.com/17160-sun-atmosphere.html</ref>
	* '''Core''': The inner 1/5th of the Sun's radius is known as it's core. Within the core is where [[nuclear fusion]] takes place, and thus it is where the energy from the Sun originates. The core has a high concentration of hydrogen [[atom]]s being pushed towards the center of the Sun as a result of [[gravity]]. When a large number of hydrogen atoms are forced into a small region, they get hot - a [[temperature]] of about 13.6 ''million'' ~~degrees~~ inside the core. When the hydrogen is heated to these temperatures they move faster and faster, colliding with each other more frequently. When fast moving hydrogen atoms collide, they will sometimes initiate a [[nuclear fusion]] reaction through the use of [[quantum tunneling]].		* '''Core''': The inner 1/5th of the Sun's radius is known as it's core. Within the core is where [[nuclear fusion]] takes place, and thus it is where the energy from the Sun originates. The core has a high concentration of hydrogen [[atom]]s being pushed towards the center of the Sun as a result of [[gravity]]. When a large number of hydrogen atoms are forced into a small region, they get hot - a [[temperature]] of about 13.6 ''million'' Kelvin inside the core. When the hydrogen is heated to these temperatures they move faster and faster, colliding with each other more frequently. When fast moving hydrogen atoms collide, they will sometimes initiate a [[nuclear fusion]] reaction through the use of [[quantum tunneling]].
	* '''Radiative Zone''': This layer is the zone that surrounds the core. The energy generated by the nuclear fusion process in the core is in the form of high energy [[photon]]s. These photons move outwards through a [[radiation\|radiative]] process.<ref>National Earth Sciences Teachers Association. (July 31, 2015). ''The Sun's Radiative Zone'' [Online]. Available: http://www.windows2universe.org/sun/Solar_interior/Sun_layers/radiative_zone.html</ref> These photons move quickly - at the [[speed of light]] - but their frequent collision with other particles results in very slow movement out of the radiative zone because they do not take a straight path outward.		* '''Radiative Zone''': This layer is the zone that surrounds the core. The energy generated by the nuclear fusion process in the core is in the form of high energy [[photon]]s. These photons move outwards through a [[radiation\|radiative]] process.<ref>National Earth Sciences Teachers Association. (July 31, 2015). ''The Sun's Radiative Zone'' [Online]. Available: http://www.windows2universe.org/sun/Solar_interior/Sun_layers/radiative_zone.html</ref> These photons move quickly - at the [[speed of light]] - but their frequent collision with other particles results in very slow movement out of the radiative zone because they do not take a straight path outward.
	*'''Convection Zone''': This area forms the outer shell of the Sun. Energy is transferred very quickly in this zone through [[convection]]. Hotter gas from the radiative zone expands and rises through the convection zone. It can do this because the convective zone is cooler than the radiative zone, and therefore less [[density\|dense]]. As the [[gas]] rises it also cools, sinking back down. As it gets closer to the radiative zone it heats up again and rises. This process repeats, creating convection currents.		*'''Convection Zone''': This area forms the outer shell of the Sun. Energy is transferred very quickly in this zone through [[convection]]. Hotter gas from the radiative zone expands and rises through the convection zone. It can do this because the convective zone is cooler than the radiative zone, and therefore less [[density\|dense]]. As the [[gas]] rises it also cools, sinking back down. As it gets closer to the radiative zone it heats up again and rises. This process repeats, creating convection currents.
	*'''Photosphere''': This portion of the Sun is a thin layer, and it is the layer where the light is emitted. Thus the photosphere is the layer of the Sun that we see from Earth.		*'''Photosphere''': This portion of the Sun is a thin layer, and it is the layer where the light is emitted. Thus the photosphere is the layer of the Sun that we see from Earth.
	*'''Chromosphere''': This is reddish-orange layer of gas. Generally it cannot be seen by the naked eye as the [[light]] from the photosphere overpowers it. However, during a solar eclipse it can be seen. It can also be seen in prominences.		*'''Chromosphere''': This is reddish-orange layer of gas. Generally it cannot be seen by the naked eye as the [[light]] from the photosphere overpowers it. However, during a solar eclipse it can be seen. It can also be seen in prominences.
	*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona ~~can approach two~~ million ~~degrees~~.		*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona are often more than one million kelvin.

	<html>		<html>
	<iframe src="https://solarsystem.nasa.gov/gltf_embed/2352" width="100%" height="450px" frameborder="0" /></iframe></html>		<iframe src="https://solarsystem.nasa.gov/gltf_embed/2352" width="100%" height="450px" frameborder="0" /></iframe></html>
	Figure 2. This is a three dimensional model of the Sun provided by NASA.<ref>NASA available online herE: https://solarsystem.nasa.gov/resources/2352/sun-3d-model/ accessed July 31st, 2020.</ref> Drag the image around to look at the Sun from different angles.		Figure 2. This is a three dimensional model of the Sun provided by NASA.<ref>NASA available online herE: https://solarsystem.nasa.gov/resources/2352/sun-3d-model/ accessed July 31st, 2020.</ref> Drag the image around to look at the Sun from different angles.


	==For further reading==		==For further reading==

Jmdonev at 17:46, 31 July 2020

2020-07-31T17:46:04Z

← Older revision		Revision as of 17:46, 31 July 2020
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	<html>		<html>
	<iframe src="https://solarsystem.nasa.gov/gltf_embed/2352" width="100%" height="450px" frameborder="0" /></iframe></html>		<iframe src="https://solarsystem.nasa.gov/gltf_embed/2352" width="100%" height="450px" frameborder="0" /></iframe></html>
	Figure 2. This is a three dimensional model of the ~~sun~~ provided by NASA.<ref>NASA available online herE: https://solarsystem.nasa.gov/resources/2352/sun-3d-model/ accessed July 31st, 2020.</ref> Drag the image around to look at the Sun from different angles.		Figure 2. This is a three dimensional model of the Sun provided by NASA.<ref>NASA available online herE: https://solarsystem.nasa.gov/resources/2352/sun-3d-model/ accessed July 31st, 2020.</ref> Drag the image around to look at the Sun from different angles.

	==For further reading==		==For further reading==

Jmdonev at 17:45, 31 July 2020

2020-07-31T17:45:20Z

← Older revision		Revision as of 17:45, 31 July 2020
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	*'''Chromosphere''': This is reddish-orange layer of gas. Generally it cannot be seen by the naked eye as the [[light]] from the photosphere overpowers it. However, during a solar eclipse it can be seen. It can also be seen in prominences.		*'''Chromosphere''': This is reddish-orange layer of gas. Generally it cannot be seen by the naked eye as the [[light]] from the photosphere overpowers it. However, during a solar eclipse it can be seen. It can also be seen in prominences.
	*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona can approach two million degrees.		*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona can approach two million degrees.

			<html>
			<iframe src="https://solarsystem.nasa.gov/gltf_embed/2352" width="100%" height="450px" frameborder="0" /></iframe></html>
			Figure 2. This is a three dimensional model of the sun provided by NASA.<ref>NASA available online herE: https://solarsystem.nasa.gov/resources/2352/sun-3d-model/ accessed July 31st, 2020.</ref> Drag the image around to look at the Sun from different angles.

	==For further reading==		==For further reading==

Jmdonev: 1 revision imported

2018-07-21T01:13:05Z

1 revision imported

← Older revision	Revision as of 01:13, 21 July 2018
(No difference)

Jmdonev at 19:20, 19 July 2018

2018-07-19T19:20:33Z

← Older revision		Revision as of 19:20, 19 July 2018
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	[[Category:Done ~~2016~~-04-30]]		[[Category:Done 2018-07-20]]
	[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]		[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]
	<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about ~~75%~~ of its total [[mass]] - and [[helium]] - about ~~25%~~ of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>		<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about three quarters of its total [[mass]] - and [[helium]] - about one quarter of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>

	==Energy from the Sun==		==Energy from the Sun==
	The [[solar energy\|energy from the Sun]] is vital to life on Earth. Not only does it allow life to exist, but it also is the source of most [[energy]] humans use. [[Biomass]], [[fossil fuel]]s, and some renewable energies such as [[wind power\|wind]] and [[solar power]] originate from the Sun. Fossil fuels are simply solar energy [[primary fuel\|stored]] in a secondary form.<ref name="RE2">What You Need to Know About Energy. (July 31, 2015). ''Our Energy Sources: The Sun'' [Online]. Available: http://needtoknow.nas.edu/energy/energy-sources/the-sun/</ref> The original energy from the Sun is captured through [[photosynthesis]] and stored in [[chemical]] bonds as plants grow. This energy is then released millions of years later after these plants have ~~decayed~~ into fossil fuels. ~~Because of this,~~ [[sunlight]] ~~is a predominant and large energy source~~. The [[solar energy to the Earth]] is significant, even after passing through hundreds of [[kilometer]]s of the Earth's [[atmosphere]]. The [[solar radiation]] that reaches the Earth has a significant amount of energy. At full intensity, the [[solar energy to the Earth]] is about 1367 W/m<sup>2</sup>.<ref>ITACA. (August 4, 2015). ''The Sun as a Source of Energy'' [Online]. Available: http://www.itacanet.org/the-sun-as-a-source-of-energy/part-2-solar-energy-reaching-the-earths-surface/</ref> Taking into account the fact that only half of the Earth faces the Sun, as well as accounting for the different amounts of sunlight that hit different latitudes, the average ~~energy~~ amounts to around 340 W/m<sup>2</sup>.		The [[solar energy\|energy from the Sun]] is vital to life on Earth. Not only does it allow life to exist, but it also is the source of most [[energy]] humans use. [[Biomass]], [[fossil fuel]]s, and some renewable energies such as [[wind power\|wind]] and [[solar power]] originate from the Sun. Fossil fuels are simply solar energy [[primary fuel\|stored]] in a secondary form.<ref name="RE2">What You Need to Know About Energy. (July 31, 2015). ''Our Energy Sources: The Sun'' [Online]. Available: http://needtoknow.nas.edu/energy/energy-sources/the-sun/</ref> The original energy from the Sun is captured through [[photosynthesis]] and stored in [[chemical]] bonds as plants grow. This energy is then released millions of years later after these plants have transformed into fossil fuels. All fossil fuels are ultimately energy from [[sunlight]]. The [[solar energy to the Earth]] is significant, even after passing through hundreds of [[kilometer]]s of the Earth's [[atmosphere]]. The [[solar radiation]] that reaches the Earth has a significant amount of energy. At full intensity, the [[solar energy to the Earth\|solar power to the Earth]] at the surface of the upper atmosphere is about 1367 W/m<sup>2</sup>.<ref>ITACA. (August 4, 2015). ''The Sun as a Source of Energy'' [Online]. Available: http://www.itacanet.org/the-sun-as-a-source-of-energy/part-2-solar-energy-reaching-the-earths-surface/</ref> Taking into account the fact that only half of the Earth faces the Sun, as well as accounting for the different amounts of sunlight that hit different latitudes and the amount of atmosphere the sunlight has to pass through, the average power amounts to around 340 W/m<sup>2</sup>.

	In addition to providing energy, the Sun's energy warms the Earth to a point that it is habitable (the [[layers of the atmosphere\|structure of the atmosphere]] also helps to ensure that the [[Earth's energy budget]] maintains a constant, livable temperature). The Sun also creates [[weather]] patterns, [[ocean current]]s, and [[air]] currents.<ref name="RE2"/>		In addition to providing energy, the Sun's energy warms the Earth to a point that it is habitable (the [[layers of the atmosphere\|structure of the atmosphere]] also helps to ensure that the [[Earth's energy budget]] maintains a constant, livable temperature). The Sun also creates [[weather]] patterns, [[ocean current]]s, and [[air]] currents.<ref name="RE2"/>
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	==Layers of the Sun==		==Layers of the Sun==
	Satellites have been launched to study the Sun continually. These satellites observe the Sun in a variety of [[wavelength]]s that helps to create a picture that describes the inner workings of the Sun. The Sun is believed to be made up of 6 different regions:<ref>Tim Sharp. (July 31, 2015). ''Atmosphere of the Sun'' [Online]. Available: http://www.space.com/17160-sun-atmosphere.html</ref>		Satellites have been launched to study the Sun continually. These satellites observe the Sun in a variety of [[wavelength]]s that helps to create a picture that describes the inner workings of the Sun. The Sun is believed to be made up of 6 different regions:<ref>Tim Sharp. (July 31, 2015). ''Atmosphere of the Sun'' [Online]. Available: http://www.space.com/17160-sun-atmosphere.html</ref>
	* '''Core''': The inner 1/5th of the Sun's radius is known as it's core. Within the core is where [[nuclear fusion]] takes place, and thus it is where the energy from the Sun originates. The core has a high concentration of hydrogen [[atom]]s being pushed towards the center of the Sun as a result of [[gravity]]. When a large number of hydrogen atoms are forced into a small region, they get hot - a [[temperature]] of about 13.6 ''million'' degrees inside the core. When the hydrogen is heated to these temperatures they move faster and faster, colliding with each other more frequently. When fast moving hydrogen atoms collide, they will sometimes initiate a nuclear fusion reaction.		* '''Core''': The inner 1/5th of the Sun's radius is known as it's core. Within the core is where [[nuclear fusion]] takes place, and thus it is where the energy from the Sun originates. The core has a high concentration of hydrogen [[atom]]s being pushed towards the center of the Sun as a result of [[gravity]]. When a large number of hydrogen atoms are forced into a small region, they get hot - a [[temperature]] of about 13.6 ''million'' degrees inside the core. When the hydrogen is heated to these temperatures they move faster and faster, colliding with each other more frequently. When fast moving hydrogen atoms collide, they will sometimes initiate a [[nuclear fusion]] reaction through the use of [[quantum tunneling]].
	* '''Radiative Zone''': This layer is the zone that surrounds the core. The energy generated by the nuclear fusion process in the core is in the form of high energy [[photon]]s. These photons move outwards through a [[radiation\|radiative]] process.<ref>National Earth Sciences Teachers Association. (July 31, 2015). ''The Sun's Radiative Zone'' [Online]. Available: http://www.windows2universe.org/sun/Solar_interior/Sun_layers/radiative_zone.html</ref> These photons move quickly - at the [[speed of light]] - but their frequent collision with other particles results in very slow movement out of the radiative zone because they do not take a straight path outward.		* '''Radiative Zone''': This layer is the zone that surrounds the core. The energy generated by the nuclear fusion process in the core is in the form of high energy [[photon]]s. These photons move outwards through a [[radiation\|radiative]] process.<ref>National Earth Sciences Teachers Association. (July 31, 2015). ''The Sun's Radiative Zone'' [Online]. Available: http://www.windows2universe.org/sun/Solar_interior/Sun_layers/radiative_zone.html</ref> These photons move quickly - at the [[speed of light]] - but their frequent collision with other particles results in very slow movement out of the radiative zone because they do not take a straight path outward.
	*'''Convection Zone''': This area forms the outer shell of the Sun. Energy is transferred very quickly in this zone through [[convection]]. Hotter gas from the radiative zone expands and rises through the convection zone. It can do this because the convective zone is cooler than the radiative zone, and therefore less [[density\|dense]]. As the [[gas]] rises it also cools, sinking back down. As it gets closer to the radiative zone it heats up again and rises. This process repeats, creating convection currents.		*'''Convection Zone''': This area forms the outer shell of the Sun. Energy is transferred very quickly in this zone through [[convection]]. Hotter gas from the radiative zone expands and rises through the convection zone. It can do this because the convective zone is cooler than the radiative zone, and therefore less [[density\|dense]]. As the [[gas]] rises it also cools, sinking back down. As it gets closer to the radiative zone it heats up again and rises. This process repeats, creating convection currents.
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	*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona can approach two million degrees.		*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona can approach two million degrees.

	==~~Additional Information~~==		==For further reading==
	For more information on the energy that comes from the Sun, see:		For more information on the energy that comes from the Sun, see:
	* [[Nuclear fusion in the Sun]]		* [[Nuclear fusion in the Sun]]
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	==References==		==References==
	{{reflist}}[[Category:Uploaded]]		{{reflist}}[[Category:Uploaded]]
	~~[[category: Ed edit]]~~

Jmdonev: 1 revision imported: From the summer

2016-09-17T22:29:24Z

1 revision imported: From the summer

← Older revision	Revision as of 22:29, 17 September 2016
(No difference)

Jmdonev at 22:12, 25 June 2016

2016-06-25T22:12:12Z

← Older revision		Revision as of 22:12, 25 June 2016
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	[[Category:Done ~~2015~~-08-21]]		[[Category:Done 2016-04-30]]
	[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]		[[File:9103296900_0d383feabf_z.jpg\|360px\|thumb\|right\|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]
	<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about 73% of its total [[mass]] - and [[helium]] - about 25% of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>		<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about 75% of its total [[mass]] - and [[helium]] - about 25% of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin\|K]] ([[celsius\|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>

	==Energy from the Sun==		==Energy from the Sun==
	The [[solar energy\|energy from the Sun]] is vital to life on Earth. Not only does it allow life to exist, but it also is the source of most [[energy]] humans use. [[Biomass]], [[fossil fuel]]s, and some renewable energies such as [[wind power\|wind]] and [[solar power]] originate from the Sun. Fossil fuels are simply solar energy in a secondary form.<ref name="RE2">What You Need to Know About Energy. (July 31, 2015). ''Our Energy Sources: The Sun'' [Online]. Available: http://needtoknow.nas.edu/energy/energy-sources/the-sun/</ref> The original energy from the Sun is captured through [[photosynthesis]] and stored in [[chemical]] bonds as plants grow. This energy is then released millions of years later after these plants have decayed into fossil fuels. Because of this, [[sunlight]] is a predominant and large energy source. The [[solar energy to the Earth]] is significant, even after passing through hundreds of [[kilometer]]s of the Earth's [[atmosphere]]. The [[solar radiation]] that reaches the Earth has a significant amount of energy. At full intensity, the [[solar energy to the Earth]] is about 1367 W/m<sup>2</sup>.<ref>ITACA. (August 4, 2015). ''The Sun as a Source of Energy'' [Online]. Available: http://www.itacanet.org/the-sun-as-a-source-of-energy/part-2-solar-energy-reaching-the-earths-surface/</ref> Taking into account the fact that only half of the Earth faces the Sun, as well as accounting for the different amounts of sunlight that hit different latitudes, the average energy amounts to around 340 W/m<sup>2</sup>.		The [[solar energy\|energy from the Sun]] is vital to life on Earth. Not only does it allow life to exist, but it also is the source of most [[energy]] humans use. [[Biomass]], [[fossil fuel]]s, and some renewable energies such as [[wind power\|wind]] and [[solar power]] originate from the Sun. Fossil fuels are simply solar energy [[primary fuel\|stored]] in a secondary form.<ref name="RE2">What You Need to Know About Energy. (July 31, 2015). ''Our Energy Sources: The Sun'' [Online]. Available: http://needtoknow.nas.edu/energy/energy-sources/the-sun/</ref> The original energy from the Sun is captured through [[photosynthesis]] and stored in [[chemical]] bonds as plants grow. This energy is then released millions of years later after these plants have decayed into fossil fuels. Because of this, [[sunlight]] is a predominant and large energy source. The [[solar energy to the Earth]] is significant, even after passing through hundreds of [[kilometer]]s of the Earth's [[atmosphere]]. The [[solar radiation]] that reaches the Earth has a significant amount of energy. At full intensity, the [[solar energy to the Earth]] is about 1367 W/m<sup>2</sup>.<ref>ITACA. (August 4, 2015). ''The Sun as a Source of Energy'' [Online]. Available: http://www.itacanet.org/the-sun-as-a-source-of-energy/part-2-solar-energy-reaching-the-earths-surface/</ref> Taking into account the fact that only half of the Earth faces the Sun, as well as accounting for the different amounts of sunlight that hit different latitudes, the average energy amounts to around 340 W/m<sup>2</sup>.

	In addition to providing energy, the Sun's energy warms the Earth to a point that it is ~~inhabitable~~ (the [[layers of the atmosphere\|structure of the atmosphere]] also helps to ensure that the [[Earth's energy budget]] maintains a constant, livable temperature). The Sun also creates [[weather]] patterns, [[ocean current]]s, and [[air]] currents.<ref name="RE2"/>		In addition to providing energy, the Sun's energy warms the Earth to a point that it is habitable (the [[layers of the atmosphere\|structure of the atmosphere]] also helps to ensure that the [[Earth's energy budget]] maintains a constant, livable temperature). The Sun also creates [[weather]] patterns, [[ocean current]]s, and [[air]] currents.<ref name="RE2"/>

	==Layers of the Sun==		==Layers of the Sun==
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	==References==		==References==
	{{reflist}}[[Category:Uploaded]]		{{reflist}}[[Category:Uploaded]]
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[[File:9103296900_0d383feabf_z.jpg|360px|thumb|right|Figure 1. An image of the Sun.<ref>NASA Goddard Space Flight Center. (July 30, 2015). ''The Sun'' [Online]. Available: https://www.flickr.com/photos/gsfc/</ref>]]
<onlyinclude>The '''Sun''' is the star at the center of our solar system. It is mostly [[hydrogen]] - about 73% of its total [[mass]] - and [[helium]] - about 25% of its total mass.</onlyinclude><ref name="RE1">Space. (July 31, 2015). ''What is Our Sun Made of?'' [Online]. Available: http://www.space.com/14745-sun-composition.html</ref> The remainder of its mass is other elements found in much smaller quantity adding up to just under two percent of the sun's mass. These elements include [[carbon]], [[nitrogen]], [[oxygen]], [[neon]], [[magnesium]], [[silicon]], [[sulfur]], and [[iron]]. Over 50 other elements are found in trace amounts. The temperature of the Sun's surface is 5778 [[kelvin|K]] ([[celsius|5505°C]]).<ref>NASA. (August 4, 2015). ''Sun Fact Sheet'' [Online]. Available: http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html</ref>

==Energy from the Sun==
The [[solar energy|energy from the Sun]] is vital to life on Earth. Not only does it allow life to exist, but it also is the source of most [[energy]] humans use. [[Biomass]], [[fossil fuel]]s, and some renewable energies such as [[wind power|wind]] and [[solar power]] originate from the Sun. Fossil fuels are simply solar energy in a secondary form.<ref name="RE2">What You Need to Know About Energy. (July 31, 2015). ''Our Energy Sources: The Sun'' [Online]. Available: http://needtoknow.nas.edu/energy/energy-sources/the-sun/</ref> The original energy from the Sun is captured through [[photosynthesis]] and stored in [[chemical]] bonds as plants grow. This energy is then released millions of years later after these plants have decayed into fossil fuels. Because of this, [[sunlight]] is a predominant and large energy source. The [[solar energy to the Earth]] is significant, even after passing through hundreds of [[kilometer]]s of the Earth's [[atmosphere]]. The [[solar radiation]] that reaches the Earth has a significant amount of energy. At full intensity, the [[solar energy to the Earth]] is about 1367 W/m<sup>2</sup>.<ref>ITACA. (August 4, 2015). ''The Sun as a Source of Energy'' [Online]. Available: http://www.itacanet.org/the-sun-as-a-source-of-energy/part-2-solar-energy-reaching-the-earths-surface/</ref> Taking into account the fact that only half of the Earth faces the Sun, as well as accounting for the different amounts of sunlight that hit different latitudes, the average energy amounts to around 340 W/m<sup>2</sup>.

In addition to providing energy, the Sun's energy warms the Earth to a point that it is inhabitable (the [[layers of the atmosphere|structure of the atmosphere]] also helps to ensure that the [[Earth's energy budget]] maintains a constant, livable temperature). The Sun also creates [[weather]] patterns, [[ocean current]]s, and [[air]] currents.<ref name="RE2"/>

==Layers of the Sun==
Satellites have been launched to study the Sun continually. These satellites observe the Sun in a variety of [[wavelength]]s that helps to create a picture that describes the inner workings of the Sun. The Sun is believed to be made up of 6 different regions:<ref>Tim Sharp. (July 31, 2015). ''Atmosphere of the Sun'' [Online]. Available: http://www.space.com/17160-sun-atmosphere.html</ref>
* '''Core''': The inner 1/5th of the Sun's radius is known as it's core. Within the core is where [[nuclear fusion]] takes place, and thus it is where the energy from the Sun originates. The core has a high concentration of hydrogen [[atom]]s being pushed towards the center of the Sun as a result of [[gravity]]. When a large number of hydrogen atoms are forced into a small region, they get hot - a [[temperature]] of about 13.6 ''million'' degrees inside the core. When the hydrogen is heated to these temperatures they move faster and faster, colliding with each other more frequently. When fast moving hydrogen atoms collide, they will sometimes initiate a nuclear fusion reaction.
* '''Radiative Zone''': This layer is the zone that surrounds the core. The energy generated by the nuclear fusion process in the core is in the form of high energy [[photon]]s. These photons move outwards through a [[radiation|radiative]] process.<ref>National Earth Sciences Teachers Association. (July 31, 2015). ''The Sun's Radiative Zone'' [Online]. Available: http://www.windows2universe.org/sun/Solar_interior/Sun_layers/radiative_zone.html</ref> These photons move quickly - at the [[speed of light]] - but their frequent collision with other particles results in very slow movement out of the radiative zone because they do not take a straight path outward.
*'''Convection Zone''': This area forms the outer shell of the Sun. Energy is transferred very quickly in this zone through [[convection]]. Hotter gas from the radiative zone expands and rises through the convection zone. It can do this because the convective zone is cooler than the radiative zone, and therefore less [[density|dense]]. As the [[gas]] rises it also cools, sinking back down. As it gets closer to the radiative zone it heats up again and rises. This process repeats, creating convection currents.
*'''Photosphere''': This portion of the Sun is a thin layer, and it is the layer where the light is emitted. Thus the photosphere is the layer of the Sun that we see from Earth.
*'''Chromosphere''': This is reddish-orange layer of gas. Generally it cannot be seen by the naked eye as the [[light]] from the photosphere overpowers it. However, during a solar eclipse it can be seen. It can also be seen in prominences.
*'''Corona''': This is a faint layer of [[plasma]] surrounding the surface of the Sun. It can only been seen with the naked eye during a solar eclipse. Temperatures in the corona can approach two million degrees.

==Additional Information==
For more information on the energy that comes from the Sun, see:
* [[Nuclear fusion in the Sun]]
* [[Solar radiation]]
* [[Insolation]]
For more information on how this energy is important on Earth, see:
* [[Solar energy to the Earth]]
* [[Temperature of the Earth]]
* [[Solar power]]

==References==
{{reflist}}[[Category:Uploaded]]