• Mechanics
    • —
      • M1. Vectors vs. Vector Quantities; Scalars vs. Scalar Quantities
      • M2. Significance of Newton’s First Law
      • M3. Newton’s Third Law: Its Formulation, Its Significance
      • M4. Momentum Conservation; Its Central Role
      • M5. Space Homogeneity And Momentum Conservation
      • M6. Inertial Mass
      • M7. Gravitational Mass
    • —
      • M8. Angular Momentum Characteristics
      • M9. Vanishing Of Total Internal Torque
      • M10. The Isotropy Of Space And Angular-Momentum Conservation
      • M11. Energy, A Central Concept
      • M12. Work And Its Relation To Kinetic And Potential Energy
      • M13. From Kepler’s Laws To Universal Gravitation
      • M14. Error And Uncertainty Distinguished
  • Thermodynamics
    • —
      • T1. What Is Thermodynamics
      • T2. Heat Vs. Internal Energy
      • T3. Equipartition And Degrees Of Freedom
      • T4. Frozen Degrees Of Freedom
      • T5. Six Versions Of The Second Law Of Thermodynamics
    • —
      • T6. Available And Unavailable Energy
      • T7. Entropy On Two Levels
      • T8. Subtleties Of Entropy
      • T9. The Arrow Of Time
  • Electricity & Magnetism
    • —
      • E1. Charge
      • E2. Early Links Between Electricity And Magnetism
      • E3. Monopoles, Not!
      • E4. The Q-ℰ-ℬ Triangle
    • —
      • E5. Inductance
      • E6. The Nature Of Light
      • E7. Why Light Travels At Speed C
      • E8. Notes On The History Of Electromagnetism
  • Relativity
    • —
      • R1. Agreement And Disagreement: Relativistic And Classical
      • R2. Transformations: Galilean And Lorentz
      • R3. “Michelson Airspeed Indicator”
      • R4. c = Constant Means Time Must Be Relative
      • R5. More Relativity And More Invariance
      • R6. E = mc2 As Einstein Derived It
    • —
      • R7. Momentum In Relativity, And Another Approach To E = mc2
      • R8. The Fourth Dimension: Spacetime And Momenergy
      • R9. Versions Of The Twin Paradox
      • R10. The Principle Of Equivalence
      • R11. Geometrodynamics
  • Quantum Physics
    • —
      • Q1. Five Key Ideas Of Quantum Mechanics
      • Q2. Granularity
      • Q3. Probability
      • Q4. Annihilation And Creation
      • Q5. Waves And Particles (The de Broglie Equation)
      • Q6. The Uncertainty Principle
      • Q7. Why Is The Hydrogen Atom As Big As It Is?
      • Q8. Localization Of Waves; Relation To Uncertainty Principle
    • —
      • Q9. Planck’s Quantum Not Yet A Photon
      • Q10. Planck’s Constant As The Particle-Wave Link
      • Q11. The Bohr Atom: Obsolete But Important
      • Q12. Bohr’s Key Atomic Postulates
      • Q13. Bohr’s Triumph: Explaining The Rydberg Constant
      • Q14. H-Atom Wave Functions And Classical Correspondence
      • Q15. The Jovian Task: Building The Atoms
      • Q16. Feynman Diagrams
  • Nuclear Physics
    • —
      • N1. Why Are There No Electrons In The Nucleus?
      • N2. The Line Of Nuclear Stability Bends And Ends
      • N3. The “Miracle” Of Nuclear Stability
      • N4. Pauli Letter Proposing What Came To Be Called The Neutrino
    • —
      • N5. Early History Of Radioactivity And Transmutation
      • N6. Bohr-Wheeler Theory Of Fission
      • N7. Sun’s Proton-Proton Cycle
  • General, Historical, Philosophical
    • —
      • G1. Faith In Simplicity As A Driver Of Science
      • G2. Science: Creation Vs. Discovery
      • G3. Is There A Scientific Method?
      • G4. What Is A Theory?
      • G5. The “Great Theories” Of Physics
      • G6. Natural Units, Dimensionless Physics
      • G7. Three Kinds Of Probability
      • G8. The Forces Of Nature
      • G9. Laws That Permit, Laws That Prohibit
    • —
      • G10. Conservation Laws, Absolute And Partial
      • G11. Math As A Tool And A Toy
      • G12. The “System Of The World”: How The Heavens Drove Mechanics
      • G13. The Astromical World, Then And Now
      • G14. Superposition
      • G15. Physics At The End Of The Nineteenth Century: The Seeds Of Rel & QM
      • G16. The Submicroscopic Frontier: Reductionism
      • G17. Submicroscopic Chaos
      • G18. The Future Path Of Science
  • Supplemental
    • Rainbows: Figuring Their Angles
  • Index
Basic PhysicsBasic Physics
A Resource for Teachers by Ken Ford
  • Mechanics
    • —
      • M1. Vectors vs. Vector Quantities; Scalars vs. Scalar Quantities
      • M2. Significance of Newton’s First Law
      • M3. Newton’s Third Law: Its Formulation, Its Significance
      • M4. Momentum Conservation; Its Central Role
      • M5. Space Homogeneity And Momentum Conservation
      • M6. Inertial Mass
      • M7. Gravitational Mass
    • —
      • M8. Angular Momentum Characteristics
      • M9. Vanishing Of Total Internal Torque
      • M10. The Isotropy Of Space And Angular-Momentum Conservation
      • M11. Energy, A Central Concept
      • M12. Work And Its Relation To Kinetic And Potential Energy
      • M13. From Kepler’s Laws To Universal Gravitation
      • M14. Error And Uncertainty Distinguished
  • Thermodynamics
    • —
      • T1. What Is Thermodynamics
      • T2. Heat Vs. Internal Energy
      • T3. Equipartition And Degrees Of Freedom
      • T4. Frozen Degrees Of Freedom
      • T5. Six Versions Of The Second Law Of Thermodynamics
    • —
      • T6. Available And Unavailable Energy
      • T7. Entropy On Two Levels
      • T8. Subtleties Of Entropy
      • T9. The Arrow Of Time
  • Electricity & Magnetism
    • —
      • E1. Charge
      • E2. Early Links Between Electricity And Magnetism
      • E3. Monopoles, Not!
      • E4. The Q-ℰ-ℬ Triangle
    • —
      • E5. Inductance
      • E6. The Nature Of Light
      • E7. Why Light Travels At Speed C
      • E8. Notes On The History Of Electromagnetism
  • Relativity
    • —
      • R1. Agreement And Disagreement: Relativistic And Classical
      • R2. Transformations: Galilean And Lorentz
      • R3. “Michelson Airspeed Indicator”
      • R4. c = Constant Means Time Must Be Relative
      • R5. More Relativity And More Invariance
      • R6. E = mc2 As Einstein Derived It
    • —
      • R7. Momentum In Relativity, And Another Approach To E = mc2
      • R8. The Fourth Dimension: Spacetime And Momenergy
      • R9. Versions Of The Twin Paradox
      • R10. The Principle Of Equivalence
      • R11. Geometrodynamics
  • Quantum Physics
    • —
      • Q1. Five Key Ideas Of Quantum Mechanics
      • Q2. Granularity
      • Q3. Probability
      • Q4. Annihilation And Creation
      • Q5. Waves And Particles (The de Broglie Equation)
      • Q6. The Uncertainty Principle
      • Q7. Why Is The Hydrogen Atom As Big As It Is?
      • Q8. Localization Of Waves; Relation To Uncertainty Principle
    • —
      • Q9. Planck’s Quantum Not Yet A Photon
      • Q10. Planck’s Constant As The Particle-Wave Link
      • Q11. The Bohr Atom: Obsolete But Important
      • Q12. Bohr’s Key Atomic Postulates
      • Q13. Bohr’s Triumph: Explaining The Rydberg Constant
      • Q14. H-Atom Wave Functions And Classical Correspondence
      • Q15. The Jovian Task: Building The Atoms
      • Q16. Feynman Diagrams
  • Nuclear Physics
    • —
      • N1. Why Are There No Electrons In The Nucleus?
      • N2. The Line Of Nuclear Stability Bends And Ends
      • N3. The “Miracle” Of Nuclear Stability
      • N4. Pauli Letter Proposing What Came To Be Called The Neutrino
    • —
      • N5. Early History Of Radioactivity And Transmutation
      • N6. Bohr-Wheeler Theory Of Fission
      • N7. Sun’s Proton-Proton Cycle
  • General, Historical, Philosophical
    • —
      • G1. Faith In Simplicity As A Driver Of Science
      • G2. Science: Creation Vs. Discovery
      • G3. Is There A Scientific Method?
      • G4. What Is A Theory?
      • G5. The “Great Theories” Of Physics
      • G6. Natural Units, Dimensionless Physics
      • G7. Three Kinds Of Probability
      • G8. The Forces Of Nature
      • G9. Laws That Permit, Laws That Prohibit
    • —
      • G10. Conservation Laws, Absolute And Partial
      • G11. Math As A Tool And A Toy
      • G12. The “System Of The World”: How The Heavens Drove Mechanics
      • G13. The Astromical World, Then And Now
      • G14. Superposition
      • G15. Physics At The End Of The Nineteenth Century: The Seeds Of Rel & QM
      • G16. The Submicroscopic Frontier: Reductionism
      • G17. Submicroscopic Chaos
      • G18. The Future Path Of Science
  • Supplemental
    • Rainbows: Figuring Their Angles
  • Index

G7. Three Kinds Of Probability

Based on Basic Physics Feature 76

When a spelunker starts down an unexplored cavern, she does not know how far she will get nor what she will find. When a gambler throws a pair of dice, he does not know what number will turn up. When a prospector holds his Geiger counter over a vein of uranium ore, he does not know how many radioactive particles he will count in a minute, even if he counted exactly the number in a preceding minute. These are three quite different kinds of uncertainty, and all of them are familiar to the scientist.

The spelunker cannot predict because of total ignorance of what lies ahead. She is in a situation that, so far as she knows, has never occurred before. She is like a scientist exploring an entirely new avenue of research. The scientist can make educated guesses about what might happen, but can neither say what will happen nor even assess the probability of any particular outcome of the exploration. That is a situation of uncertain knowledge and uncertain probability.

The gambler is in a better position. He has uncertain knowledge but certain probability. He knows all the possible outcomes of his throw and knows exactly the chance that any particular outcome will actually occur. His ignorance of any single result is tempered by a definite knowledge of average results.

The probability of atomic multitudes, which is the same as the probability of the gambler, lies at the heart of some of the most important aspects of the behavior of matter in bulk. This kind of probability we can call a probability of ignorance—not the nearly total ignorance of the spelunker in a new cave or the researcher on a new frontier, but the ignorance of certain details called initial conditions. If the gambler knew with enough precision every mechanical detail of the throw of the dice and the frictional properties of the surface onto which they are thrown (the initial conditions) he could (in principle) calculate exactly the outcome of the throw. Similarly, the physicist with enough precise information about the whereabouts and velocities of a collection of atoms at one time could (with an even bigger “in principle”1) calculate their exact arrangement at a later time. Because these details are lacking, probability necessarily enters the picture.

The prospector’s uncertainty is of still a different kind. He is coming up against what is, so far as we now know, a fundamental probability of nature, a probability not connected with ignorance of specific details, but rather connected with the operation of the laws of nature at the most elementary level. In atomic and nuclear events, such as radioactivity, probability plays a role, even when every possible initial condition is known. This is quantum probability (see Essay Q3). In thermodynamics—the study of the average behavior of large numbers of molecules and of the links between the submicroscopic and macroscopic worlds—the fundamental probability in nature is of only secondary importance. It influences the details of individual atomic and molecular collisions, but these details are unknown in any case. Of primary importance is the probability of ignorance stemming from our necessarily scant knowledge of precise details of molecular motion.

The triumphs of thermodynamics are its definite laws of behavior for systems about which we have incomplete knowledge. However, it should be no surprise that laws of probability applied to large enough numbers can become laws of near certainty. The owners of gambling casinos are consistent winners.


1 Because classical mechanics does not suffice to calculate exactly the outcome of an atomic collision, this hypothetical forecast of future atomic positions and velocities could be extended but a moment forward in time.


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