Difference between revisions of "Nuclear Fusion"

Revision as of 13:34, 11 March 2019

Key Stage 4

Meaning

Nuclear fusion is a process in which two small atomic nuclei join together to become a larger nucleus.

About Nuclear Fusion

For a fusion reaction to occur the two nuclei must have enough kinetic energy to overcome the electrostatic force of repulsion between the positively charged nuclei.

To provide enough kinetic energy to the nuclei the substance must be heated to a temperature of several million degrees Celsius.

Nuclear fusion occurs naturally in the centre of a Star due to the high temperatures and pressure.

Nuclear fusion is possible in laboratories on Earth but it cannot be sustained for long periods of time to produce enough energy to be useful as an energy resource.

Nuclear fusion in laboratories on Earth must be done at much higher temperature than in the centre of Stars because the centre of Stars is a much higher pressure so nuclei collide more often.

500px
Fusion of a Tritium and a Deuterium nucleus produces a Helium nucleus. \({}_1^2H + {}_1^3H \rightarrow {}_2^4He + {}_0^1n\) This is the most common pathway for nuclear fusion in Stars as the neutron goes on to be captured by a Hydrogen nucleus to become Deuterium or captured by a Deuterium nucleus to become a Tritium nucleus.


Fusion of two Hydrogen nuclei (protons) produces a Deuterium nucleus. \({}_1^1H + {}_1^1H \rightarrow {}_1^2H + {}_{-1}^0\beta\)


Fusion of a Hydrogen nucleus (proton) and a Deuterium nucleus produces a Tritium nucleus. \({}_1^1H + {}_1^2H \rightarrow {}_1^3H + {}_{-1}^0\beta\)


Fusion of two Deuterium nuclei produces a Helium nucleus. \({}_1^2H + {}_1^2H \rightarrow {}_2^4He\)


Fusion of a Hydrogen nucleus (proton) and a Tritium nucleus produces a Helium nucleus. \({}_1^1H + {}_1^3H \rightarrow {}_2^4He\)

@@ Line 9: / Line 9: @@
 : '''Nuclear fusion''' is possible in [[laboratory|laboratories]] on [[Earth]] but it cannot be sustained for long periods of [[time]] to produce enough [[energy]] to be useful as an [[Energy Resource|energy resource]].
 : '''Nuclear fusion''' in [[laboratory|laboratories]] on [[Earth]] must be done at much higher [[temperature]] than in the centre of [[Star]]s because the centre of [[Star]]s is a much higher [[pressure]] so [[Atomic Nucleus|nuclei]] collide more often.
+{| class="wikitable"
+|-
+|[[File:FusionDTH.png|center|500px]]
+|-
+| style="height:20px; width:500px; text-align:center;" |'''Fusion''' of a [[Tritium]] and a [[Deuterium]] [[Atomic Nucleus|nucleus]] produces a [[Helium]] [[Atomic Nucleus|nucleus]].
+<math>{}_1^2H + {}_1^3H \rightarrow {}_2^4He + {}_0^1n</math>
+This is the most common pathway for [[Nuclear Fusion|nuclear fusion]] in [[Star]]s as the [[neutron]] goes on to be captured by a [[Hydrogen]] [[Atomic Nucleus|nucleus]] to become [[Deuterium]] or captured by a [[Deuterium]] [[Atomic Nucleus|nucleus]] to become a [[Tritium]] [[Atomic Nucleus|nucleus]].
+|}
 {| class="wikitable"
@@ Line 24: / Line 34: @@
 | style="height:20px; width:500px; text-align:center;" |'''Fusion''' of a [[Hydrogen]] [[Atomic Nucleus|nucleus]] ([[proton]]) and a [[Deuterium]] [[Atomic Nucleus|nucleus]] produces a [[Tritium]] [[Atomic Nucleus|nucleus]].
 <math>{}_1^1H + {}_1^2H \rightarrow {}_1^3H + {}_{-1}^0\beta</math>
+|}
+{| class="wikitable"
+|-
+|[[File:FusionDDH.png|center|500px]]
+|-
+| style="height:20px; width:500px; text-align:center;" |'''Fusion''' of two [[Deuterium]] [[Atomic Nucleus|nuclei]] produces a [[Helium]] [[Atomic Nucleus|nucleus]].
+<math>{}_1^2H + {}_1^2H \rightarrow {}_2^4He</math>
+|}
+{| class="wikitable"
+|-
+|[[File:FusionPTH.png|center|500px]]
+|-
+| style="height:20px; width:500px; text-align:center;" |'''Fusion''' of a [[Hydrogen]] [[Atomic Nucleus|nucleus]] ([[proton]]) and a [[Tritium]] [[Atomic Nucleus|nucleus]] produces a [[Helium]] [[Atomic Nucleus|nucleus]].
+<math>{}_1^1H + {}_1^3H \rightarrow {}_2^4He</math>
 |}