Nuclear fusion in the Sun - Revision history

Jmdonev at 03:17, 16 June 2020

2020-06-16T03:17:40Z

← Older revision		Revision as of 03:17, 16 June 2020
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	[[Category:~~Done 2015-08-21~~]]		[[Category:Ashley edit]]
	[[File:sunfusion2.png\|360px\|thumb\|right\|Figure 1. The proton-proton fusion process that is the source of energy from the Sun.<ref>Wikimedia Commons. (July 30, 2015). ''Fusion in the Sun'' [Online]. Available:https://upload.wikimedia.org/wikipedia/commons/0/03/Fusion_in_the_Sun_it.png</ref> ]]		[[File:sunfusion2.png\|360px\|thumb\|right\|Figure 1. The proton-proton fusion process that is the source of energy from the Sun.<ref>Wikimedia Commons. (July 30, 2015). ''Fusion in the Sun'' [Online]. Available:https://upload.wikimedia.org/wikipedia/commons/0/03/Fusion_in_the_Sun_it.png</ref> ]]

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	# Two protons within the Sun fuse. Most of the time the pair breaks apart again, but sometimes one of the protons transforms into a [[neutron]] via the [[weak nuclear force]]. Along with the transformation into a neutron, a positron and neutrino are formed. This resulting proton-neutron pair that forms sometimes is known as [[deuterium]].		# Two protons within the Sun fuse. Most of the time the pair breaks apart again, but sometimes one of the protons transforms into a [[neutron]] via the [[weak nuclear force]]. Along with the transformation into a neutron, a positron and neutrino are formed. This resulting proton-neutron pair that forms sometimes is known as [[deuterium]].
	# A third proton collides with the formed deuterium. This collision results in the formation of a helium-3 nucleus and a [[gamma decay\|gamma ray]]. These gamma rays work their way out from the core of the Sun and are released as [[sunlight]].		# A third proton collides with the formed deuterium. This collision results in the formation of a helium-3 nucleus and a [[gamma decay\|gamma ray]]. These gamma rays work their way out from the core of the Sun and are released as [[sunlight]].
	# Two helium-3 nuclei collide, creating a helium-4 nucleus plus two extra ~~neutrons~~. Technically, a [[beryllium\|beryllium-6]] nuclei forms first but is unstable and thus disintegrates into the helium-4 nucleus.		# Two helium-3 nuclei collide, creating a helium-4 nucleus plus two extra protons that escape as two hydrogen. Technically, a [[beryllium\|beryllium-6]] nuclei forms first but is unstable and thus disintegrates into the helium-4 nucleus.
	The final helium-4 atom has less mass than the original 4 protons that came together (see [[E=mc2]]). Because of this, their combination results in an excess of energy being released in the form of heat and light that exits the Sun, given by the [[mass-energy equivalence]]. To exit the Sun, this energy must travel through many layers to the [[Sun#Layers of the Sun\|photosphere]] before it can actually emerge into space as sunlight. Since this proton-proton chain happens frequently - 9.2 x 10<sup>37</sup> times per second - there is a significant release of energy.<ref name="RE2"/> Of all of the [[mass]] that undergoes this fusion process, only about 0.7% of it is turned into energy. Although this seems like a small amount of mass, this is equal to 4.26 million metric [[tonne]]s of matter being converted to energy per second.<ref name="RE2"/> Using the mass-energy equivalence, we find that this 4.26 million metric tonnes of matter is equal to about 3.8 x 10<sup>26</sup> [[joule]]s of energy released per second!		The final helium-4 atom has less mass than the original 4 protons that came together (see [[E=mc2]]). Because of this, their combination results in an excess of energy being released in the form of heat and light that exits the Sun, given by the [[mass-energy equivalence]]. To exit the Sun, this energy must travel through many layers to the [[Sun#Layers of the Sun\|photosphere]] before it can actually emerge into space as sunlight. Since this proton-proton chain happens frequently - 9.2 x 10<sup>37</sup> times per second - there is a significant release of energy.<ref name="RE2"/> Of all of the [[mass]] that undergoes this fusion process, only about 0.7% of it is turned into energy. Although this seems like a small amount of mass, this is equal to 4.26 million metric [[tonne]]s of matter being converted to energy per second.<ref name="RE2"/> Using the mass-energy equivalence, we find that this 4.26 million metric tonnes of matter is equal to about 3.8 x 10<sup>26</sup> [[joule]]s of energy released per second!

	==~~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:
	* [[Sun]]		* [[Sun]]
	* [[Solar radiation]]		* [[Solar radiation]]
	* [[Insolation]]		* [[Insolation]]
	~~For more information on how this energy is important on Earth, see:~~
	* [[Solar energy to the Earth]]		* [[Solar energy to the Earth]]
	* [[Temperature of the Earth]]		* [[Temperature of the Earth]]
	* [[Solar power]]		* [[Solar power]]
			*Or explore a [[Special:Random\|random page]]

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

J.williams: 1 revision imported

2015-08-26T21:31:54Z

1 revision imported

← Older revision	Revision as of 21:31, 26 August 2015
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J.williams at 18:50, 24 August 2015

2015-08-24T18:50:45Z

New page

[[Category:Done 2015-08-21]]
[[File:sunfusion2.png|360px|thumb|right|Figure 1. The proton-proton fusion process that is the source of energy from the Sun.<ref>Wikimedia Commons. (July 30, 2015). ''Fusion in the Sun'' [Online]. Available:https://upload.wikimedia.org/wikipedia/commons/0/03/Fusion_in_the_Sun_it.png</ref> ]]

<onlyinclude>The [[energy]] from the [[Sun]] - both [[heat]] and [[light]] energy - originates from a '''[[nuclear fusion]] process''' that is occurring inside the [[Sun#Layers of the Sun|core of the Sun]]. The specific type of fusion that occurs inside of the Sun is known as '''proton-proton fusion'''.</onlyinclude><ref name="RE1">Fraser Cain. (July 30, 2015). ''Fusion in the Sun'' [Online]. Available: http://www.universetoday.com/18707/fusion-in-the-sun/</ref>

Inside the Sun, this process begins with [[proton]]s (which is simply a lone [[hydrogen]] [[nucleus]]) and through a series of steps, these protons fuse together and are turned into [[helium]]. This fusion process occurs inside the core of the Sun, and the transformation results in a release of energy that keeps the sun hot. The resulting energy is [[radiation|radiated]] out from the core of the Sun and moves across the solar system.<ref name="RE2">Jerry Coffey. (July 31, 2015). ''How Does The Sun Produce Energy?'' [Online]. Available: http://www.universetoday.com/75803/how-does-the-sun-produce-energy/</ref> It is important to note that the core is the only part of the Sun that produces any significant amount of [[heat]] through fusion (it contributes about 99%).<ref name="RE2"/> The rest of the Sun is heated by energy transferred outward from the core.

==Steps==
The overall process of proton-proton fusion within the Sun can be broken down into several simple steps. A visual representation of this process is shown in Figure 1. The steps are:<ref>Karl Tate. (July 30, 2015). ''Proton Fusion, the Sun's Power Source, Explained'' [Online]. Available: http://www.space.com/26956-proton-fusion-sun-power-source-infographic.html</ref>

# Two protons within the Sun fuse. Most of the time the pair breaks apart again, but sometimes one of the protons transforms into a [[neutron]] via the [[weak nuclear force]]. Along with the transformation into a neutron, a positron and neutrino are formed. This resulting proton-neutron pair that forms sometimes is known as [[deuterium]].
# A third proton collides with the formed deuterium. This collision results in the formation of a helium-3 nucleus and a [[gamma decay|gamma ray]]. These gamma rays work their way out from the core of the Sun and are released as [[sunlight]].
# Two helium-3 nuclei collide, creating a helium-4 nucleus plus two extra neutrons. Technically, a [[beryllium|beryllium-6]] nuclei forms first but is unstable and thus disintegrates into the helium-4 nucleus.
The final helium-4 atom has less mass than the original 4 protons that came together (see [[E=mc2]]). Because of this, their combination results in an excess of energy being released in the form of heat and light that exits the Sun, given by the [[mass-energy equivalence]]. To exit the Sun, this energy must travel through many layers to the [[Sun#Layers of the Sun|photosphere]] before it can actually emerge into space as sunlight. Since this proton-proton chain happens frequently - 9.2 x 10<sup>37</sup> times per second - there is a significant release of energy.<ref name="RE2"/> Of all of the [[mass]] that undergoes this fusion process, only about 0.7% of it is turned into energy. Although this seems like a small amount of mass, this is equal to 4.26 million metric [[tonne]]s of matter being converted to energy per second.<ref name="RE2"/> Using the mass-energy equivalence, we find that this 4.26 million metric tonnes of matter is equal to about 3.8 x 10<sup>26</sup> [[joule]]s of energy released per second!

==Additional Information==
For more information on the energy that comes from the Sun, see:
* [[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]]