Energy Conservation

POTENTIAL AND KINETIC ENERGY

What is Energy?

Energy is the ability to do work, usually against some force. When you climbed the stairs to this class, you had to do work against gravity to get up here. That required an expenditure of energy.

But, you only borrowed this energy. You can get it back if you jump back down to the atrium floor (not recommended).

Energy comes in many forms, kinetic, potential (stored), heat, etc. Energy is always conserved. It is not created or destroyed but is just transformed from one form to another.

Kinetic and Potential Energy:

Throwing a ball into the air represents a situation in which the total energy is fixed and there is a continous transformation from kinetic energy to potential energy.

Most Energy loss is via heat. This is generally not released. Heat loss is usually irrecoverable. This is a principle feature of the field of thermodynamics that we will discuss later.

Thermodynamics Primer:

THERMODYNAMIC LAWS

You can not subvert or change these laws:

The Zeroth Law (0): Systems are in equilibrium when they are at the same temperature.

The First Law (1): Energy is Conserved in a closed system:

The Second Law (2): The Law of Entropy:

To decrease local entropy requires work (energy).

But what is heat? Heat is infrared radiation.

Common Types of Energy

Type of Energy

What it is

  • Kinetic Energy (KE)
  • Gravitational Potential Energy (GPE)
  • Chemical Potential Energy (CPE)
  • Elastic Potential Energy (ELPE)
  • Thermal Energy (H)
  • Electromagnetic Radiation (ER)

  • energy associated with motion
  • energy associated with position in a gravitational field
  • energy associated with the bonding of molecules in a chemical
  • "spring energy" - a form of stored energy
  • heat dissipation
  • release of photons
  • The concept of conservation of energy will be reinforced with some classroom demonstrations today. The most important concept is to observe different systems and identify the potential sources of energy loss.

    Conservation of Energy is crucial to understanding atomic spectra and how its possible to determine that different elements are inside of stars. This will be discussed in the context of photon emission and absorption on Thursday.