Week 6 Term 2 2026 Nuclear Reactions

 Homework

Models of the Atom & Radioactivity

• Act 15A, p.173-176 Models of the Atom and Radioactivity
• Ex 5A, p. 151-155 Models of the Atom
• Ex 5B, p.160-171 Radioactivity

Nuclaer Reactions

• Act 16A, p. 181, Nuclear Reactions
• Ex 5C, p.175-182 Nuclear Reactions

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Element formation in Stars Nuclear Fusion

Binding Energy Per Nucleon

Mass Per Nucleon

A 'cheatsheet' on Binding Energy in nuclear physics

Binding Energy - A-level Physics

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Natural Nuclear Fission Reactor

Week 7 Term 2 2025 Nuclear Reactions

Homework

Models of the Atom & Radioactivity

• Act 15A, p.173-176 Models of the Atom and Radioactivity
• Ex 5A, p. 151-155 Models of the Atom
• Ex 5B, p.160-171 Radioactivity

Nuclaer Reactions

• Act 16A, p. 181, Nuclear Reactions
• Ex 5C, p.175-182 Nuclear Reactions

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Element formation in Stars Nuclear Fusion

Binding Energy Per Nucleon

Mass Per Nucleon

A 'cheatsheet' on Binding Energy in nuclear physics

Binding Energy - A-level Physics

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Natural Nuclear Fission Reactor

Week 6 Term 2 2023

  Homework

• Act 15A, p.173-176 Models of the Atom and Radioactivity
• Ex 5A, p. 151-155 Models of the Atom
• Act 16A, p. 181, Nuclear Reactions
• Ex 5B, p.160-171 Radioactivity

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Element formation in Stars Nuclear Fusion

Binding Energy Per Nucleon

Mass Per Nucleon

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Natural Nuclear Fission Reactor

Term 2 Week 11 2020

Homework

• Ex 5A, p. 151-155, Models of the Atom
• Ex 5B, p. 160-171, Radioactivity
• Ex 5C, p. 175-182, Nuclear Reactions

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Element formation in Stars Nuclear Fusion

Binding Energy Per Nucleon

Mass Per Nucleon

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Natural Nuclear Fission Reactor

Term 2 Week 7 2018

Homework

• Ex 5A, p. 151-155, Models of the Atom
• Ex 5B, p. 160-171, Radioactivity
• Ex 5C, p. 175-182, Nuclear Reactions

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Mass Energy Equivalence

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Term 2 Week 6 2017

Homework

• Ex 5A, p. 151-155, Models of the Atom
• Ex 5B, p. 160-171, Radioactivity
• Ex 5C, p. 175-182, Nuclear Reactions

Chem/Phy Canterbury Field Trip this Thursday-Friday

Nuclear Reactions:

• Conservation of Atomic Number
• Conservation of Nucleon Number
• Conservation of Mass-Energy E = Δmc2

E = Δmc2

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Mass Energy Equivalence

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion

Term 2 Week 6 2016

Homework,

• Ex 5B Radioactive Decay and Half Life - This should be complete by now
• Ex 5C Nuclear Reactions and Nuclear Energy Calculations - due next week

Nuclear Fusion in the Sun

Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons

E = Δmc2

Mass Energy Equivalence

Nuclear Reactions

Fission Fusion and Radioactive Decay

Fission & Fusion