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Here the Meissner effect is demonstrated by the levitation of a magnet above a liquid nitrogen cooled superconductor. Credit: Mai-Linh Doan.
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Physics is the study of how the universe works. It has been described as a "science that deals with matter and energy and their interactions"[1], and as the "branch of science concerned with the study of properties and interactions of space, time, matter and energy"[2].

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This article is part of the School:Physics and Astronomy

Background and history[edit]

A major thrust of physics over the last few hundred years (since the time of Galileo and Newton) has been to understand the workings of the universe in terms of ever-more-fundamental principles. This has generally involved an understanding of what a "force" means, though modern formulations of forces are very different from what they were in Newton's time.

By the middle of the 20th century, physicists recognized 4 fundamental forces:

  • gravity
  • electromagnetism
  • the "strong" nuclear force, responsible for holding nuclei together, and for nuclear power and some types of radioactivity.
  • the "weak" nuclear force, responsible for some other types of radioactivity.

One unification had already taken place in the 19th century: the previously disparate electric and magnetic forces were combined into the electromagnetic force, due to the work of Oersted, Faraday, and Maxwell.

During the 20th century, all of the forces except gravity were reformulated in terms of "gauge theories" within the framework of Quantum Mechanics. The forces act through the exchange of "gauge bosons".

In the 1970's, the electromagnetic and weak forces were unified into the "electroweak force", due to the work of Weinberg, Salam, and Glashow.

In the late 20th century, a "grand unified theory" (GUT) was developed, that unifies the electroweak and strong forces. This is often called the "standard model". It is still under development.

The "theory of everything" (TOE), that would unify the standard model with gravity, is still elusive. Efforts in this area include "string theory" and "supersymmetry".

Articles related to physics[edit]

Atomic, Nuclear and particle physics[edit]

Quantum mechanics[edit]




Classical mechanics[edit]



Mathematical physics[edit]

Since the time of Newton, mathematics has played a major role in physics. Some of the mathematical techniques are objects of study in their own right.

Time and conditions[edit]

The photograph of various lamps illustrates the effect of color temperature differences (left to right): (1) Compact Fluorescent: General Electric, 13 watt, 6500 K (2) Incandescent: Sylvania 60-Watt Extra Soft White (3) Compact Fluorescent: Bright Effects, 15 watts, 2644 K, and (4) Compact Fluorescent: Sylvania, 14 watts, 3000 K. Credit: Ramjar.

In physics, a key value on the time axis for collecting physical data is the starting time. “Incandescents reach full brightness a fraction of a second after being switched on.”[3]

Eventually it occurred to many of the intelligent life forms on Earth that in addition to where the observations of the natural objects or entities in the sky are taken, also when and how the observations are taken is important. The results of observations change with time, temperature, and other atmospheric conditions.

Many of the early laws begin to make sense and increase understanding of the phenomena observed when coupled to experimental and theoretical studies performed in a laboratory here on Earth under controlled conditions. Astronomy benefits from physics.

Laboratory conditions are often expressed in terms of standard temperature and pressure.

"Standard condition for temperature and pressure are standard sets of conditions for experimental measurements established to allow comparisons to be made between different sets of data. The most used standards are those of the International Union of Pure and Applied Chemistry (IUPAC) and the National Institute of Standards and Technology (NIST), although these are not universally accepted standards. Other organizations have established a variety of alternative definitions for their standard reference conditions."[4]

"In chemistry, IUPAC established standard temperature and pressure (informally abbreviated as STP) as a temperature of 273.15 K (0 °C, 32 °F) and an absolute pressure of 100 kPa (14.504 psi, 0.986 atm, 1 bar),[5] An unofficial, but commonly used standard is standard ambient temperature and pressure (SATP) as a temperature of 298.15 K (25 °C, 77 °F) and an absolute pressure of 100 kPa (14.504 psi, 0.986 atm). The STP and the SATP should not be confused with the standard state commonly used in thermodynamic evaluations of the Gibbs free energy of a reaction."[4]

"Standard conditions for gases: Temperature, 273.15 K [...] and pressure of 105 pascals. The previous standard absolute pressure of 1 atm (equivalent to 1.01325 × 105 Pa) was changed to 100 kPa in 1982. IUPAC recommends that the former pressure should be discontinued."[5]

"NIST uses a temperature of 20 °C (293.15 K, 68 °F) and an absolute pressure of 101.325 kPa (14.696 psi, 1 atm). The International Standard Metric Conditions for natural gas and similar fluids are 288.15 K (59.00 °F, 15.00 °C) and 101.325 kPa.[6]"[4]

Line of sight[edit]

This image shows a late-summer rainstorm in Denmark. The nearly black color of the cloud's base indicates the foreground cloud is probably cumulonimbus. Credit: Malene Thyssen.
This beautiful galaxy is tilted at an oblique angle on to our line of sight, giving a "birds-eye view" of the spiral structure. Credit: Hubble data: NASA, ESA, and A. Zezas (Harvard-Smithsonian Center for Astrophysics); GALEX data: NASA, JPL-Caltech, GALEX Team, J. Huchra et al. (Harvard-Smithsonian Center for Astrophysics); Spitzer data: NASA/JPL/Caltech/S. Willner (Harvard-Smithsonian Center for Astrophysics.

Def. “[a] straight line along which an observer has a clear view”[7] is called line of sight.

In the section on 'senses' is a demonstration of the principle of 'line of sight'; i.e., "a line from an observer's eye to a distant point toward which [the observer] is looking"[1]. In the image on the left of rain beneath a dark cloud, there is a highway with a vehicle on it. The vehicle is further away from the observer than the right turn onto a side road. Is the blue sky behind the dark cloud? Is the line of trees in the background further away than the dark cloud? Many objects in this image and the others can be layered relative to the observer (some are closer by inspection than others). These layers or strata are strata along the line of sight. The principle of line of sight can be used to make deductions about the relative locations (or positions) of objects from the observer's perspective.

By observing many of the wandering lights in the night sky, an occasional occultation of the light of one astronomical object may occur by the intervention of another along a closer astronomical stratum. On April 25, 1838, an occultation of Mercury by the Moon occurred when Mercury was visible to the unaided eye after sunset.[8] An occultation of Venus by the Moon occurred "on the afternoon of October 14", 1874.[8] An earlier such occultation "occurred on May 23, 1587, and is thus recorded by [Tycho Brahe] in his Historia Celestis"[8]. "Thomas Street, in his Astronomia Carolina (A.D. 1661), mentions three occultations by Venus, being two occasions when the planet covered Regulus, and once when there was an occultation of Mars by Venus."[8] "[Thomas Street] describes [the occultation of Mars by Venus] as follows: "1590,. Oct. 2nd, 16h. 24s. Michael Mœstlin observed ♂ eclipsed by ♀.""[8]


Cartesian coordinate system with a circle of radius 2 centered at the origin marked in red. The equation of a circle is (x - a)2 + (y - b)2 = r2 where a and b are the coordinates of the center (a, b) and r is the radius. Credit: 345Kai.

“A Cartesian coordinate system specifies each point uniquely in a plane by a pair of numerical coordinates, which are the signed distances from the point to two fixed perpendicular directed lines, measured in the same unit of length. Each reference line is called a coordinate axis or just axis of the system, and the point where they meet is its origin, usually at ordered pair (0,0). The coordinates can also be defined as the positions of the perpendicular projections of the point onto the two axes, expressed as signed distances from the origin.”[9]


Distance along a path is compared in this diagram with displacement. Credit: .

Def. "[t]he amount of space between two points, usually geographical points, usually (but not necessarily) measured along a straight line", per Wiktionary distance, is called distance.

"Distance (or farness) is a numerical description of how far apart objects are. In physics or everyday discussion, distance may refer to a physical length, or an estimation based on other criteria (e.g. "two counties over"). In mathematics, a distance function or metric is a generalization of the concept of physical distance. A metric is a function that behaves according to a specific set of rules, and provides a concrete way of describing what it means for elements of some space to be "close to" or "far away from" each other."[10]


The universe within 1 billion light-years (307 Mpc) of Earth is shown to contain the local superclusters, galaxy filaments and voids. Credit: Richard Powell.

“In set theory, emptiness is symbolized by the empty set: a set that contains no elements.”[11]

Def. “the state of being ... [d]evoid of content; containing nothing”[12] is called empty.

“Free space, a perfect vacuum as expressed in the classical physics model ... Vacuum state, a perfect vacuum based on the quantum mechanical model ... In mathematical physics, the homogeneous equation may correspond to a physical theory formulated in empty space”[13] are disambiguations for "empty space".

“In astronomy, voids are the empty spaces between filaments (the largest-scale structures in the Universe), which contain very few, or no, galaxies. ... Voids located in high-density environments are smaller than voids situated in low-density spaces of the universe.[14][15]


Def. "[a] physical quantity that denotes ability to push, pull, twist or accelerate a body which is measured in a unit dimensioned in mass × distance/time² (ML/T²): SI: newton (N); CGS: dyne (dyn)" is called force.

Def. a force "associated with nuclear decay", per Wiktionary weak nuclear force, is called the weak nuclear force.

Def. "a fundamental force that is associated with the strong bonds", from Wiktionary strong nuclear force, is called the strong nuclear force.

The key values to determine in both force and energy are \frac{L}{T^2} and \frac{L^2}{T^2}. Force (F) x distance (L) = energy (E), \frac{L}{T^2} \times L = \frac{L^2}{T^2}. Force and energy are related to distance and time using proportionality constants.

Sources of the forces[edit]

One theoretical source of a force is the presence of mass.

Newton's second law of motion is that F = ma, where F is the force applied, m is the mass of the object receiving the force, and a is the acceleration observed for the astronomical object. The newton is therefore:[16]

{1~{\rm N} = 1~{\rm kg} \frac{{\rm m}} {{\rm s}^2}}


N: newton
kg: kilogram
m: metre
s: second.
Every point mass attracts every single other point mass by a force pointing along the line intersecting both points. The force is proportional to the product of the two masses and inversely proportional to the square of the distance between them:[17]
F = G \frac{m_1 m_2}{r^2}\ ,


  • F is the force between the masses,
  • G is the gravitational constant,
  • m1 is the first mass,
  • m2 is the second mass, and
  • r is the distance between the centers of the masses.
The diagram shows two masses attracting one another. Credit: .

In the International System of Units (SI) units, F is measured in newtons (N), m1 and m2 in kilograms (kg), r in meters (m), and the constant G is approximately equal to 6.674×10−11
 N m2 kg−2

Another theoretical source of a force is charge.

Coulomb's law states that the electrostatic force F experienced by a charge, q at position r_q, in the vicinity of another charge, Q at position r_Q, in vacuum is equal to:

F = {qQ\over4\pi\varepsilon_0}{1\over {r^2}},

where \varepsilon_0 is the electric constant and r is the distance between the two charges.

Coulomb's constant is

k_e = 1 / (4\pi\varepsilon_0\varepsilon),

where the constant \varepsilon_0 is called the permittivity of free space in SI units of C2 m−2 N−1.

For reality, \varepsilon is the relative (dimensionless) permittivity of the substance in which the charges may exist.


Def. "[a] quantity that denotes the ability to do work and is measured in a unit dimensioned in mass × distance²/time² (ML²/T²) or the equivalent"[19] is called energy.

The energy E for the system in the section about forces is

E = F \cdot D,

where D is the displacement.


Def. "[a] region affected by a particular force" is called a field.

Def. "[a] region of space around a charged particle, or between two voltages; it exerts a force on charged objects in its vicinity", per Wiktionary electric field, is called an electric field.

Def. "a condition in the space around a magnet or electric current in which there is a detectable magnetic force and two magnetic poles are present", from Wiktionary magnetic field, is called a magnetic field.


Def. "The fundamental force of attraction that exists between all particles with mass in the universe", per Wiktionary gravitation, is called gravitation.


Def. "[t]he basic structural component of the universe [that] usually has mass and volume"[20] is called matter.

"In physics, mass, more specifically inertial mass, can be defined as a quantitative measure of an object's resistance to the change of its speed. In addition to this, gravitational mass can be described as a measure of magnitude of the gravitational force which is

  1. exerted by an object (active gravitational mass), or
  2. experienced by an object (passive gravitational force)

when interacting with a second object. The SI unit of mass is the kilogram (kg)."[21]


A typical tape measure with both metric and US units is shown to measure two US pennies. Credit: .

"Measurement is the process or the result of determining the ratio of a physical quantity, such as a length, time, temperature etc., to a unit of measurement, such as the meter, second or degree Celsius."[22]

Physical units[edit]

Def. "exactly 149,597,870.691 kilometres" is called one AU.[23]

Def. "86,400 SI seconds (s)" is called 1 day (d).[23]

Def. "1.9891 x 1030 kg" is called the mass of the Sun.[23]

Def. "9,460,730,472,580.8 km" is called the light-year (ly).[23]


"In nuclear physics and nuclear chemistry, nuclear fission refers to either a nuclear reaction or a radioactive decay process in which the nucleus of an atom splits into smaller parts (lighter nuclei), often producing free neutrons and photons (in the form of gamma rays), and releasing a very large amount of energy, even by the energetic standards of radioactive decay. The two nuclei produced are most often of comparable but slightly different sizes, typically with a mass ratio of products of about 3 to 2, for common fissile isotopes.[24][25] Most fissions are binary fissions, but occasionally (2 to 4 times per 1000 events), three positively charged fragments are produced in a ternary fission. The smallest of these ranges in size from a proton to an argon nucleus." from the Wikipedia article on nuclear fission.


From the Wikipedia article on nuclear fusion, "Nuclear fusion is the process by which two or more atomic nuclei join together, or "fuse", to form a single heavier nucleus. This is usually accompanied by the release or absorption of large quantities of energy. Fusion is the process that powers active stars, the hydrogen bomb and some experimental devices examining fusion power for electrical generation. The fusion of two nuclei with lower masses than iron (which, along with nickel, has the largest binding energy per nucleon) generally releases energy, while the fusion of nuclei heavier than iron absorbs energy. The opposite is true for the reverse process, nuclear fission. This means that fusion generally occurs for lighter elements only, and likewise, that fission normally occurs only for heavier elements. There are extreme astrophysical events that can lead to short periods of fusion with heavier nuclei. This is the process that gives rise to nucleosynthesis, the creation of the heavy elements during events such as supernovas."


The electromagnetic spectrum. The red line indicates the room temperature thermal energy. Credit: Opensource Handbook of Nanoscience and Nanotechnology.

Def. an action or process of throwing or sending out a traveling ray in a line, beam, or stream of small cross section is called radiation, from radiation astronomy.

The term radiation is often used to refer to the ray itself.

Radiation comes in many forms and energies.

Notation: let various International System of Units, SI prefixes, occur before the unit of energy, the electronvolt, abbreviated as eV.

For example, PeV denotes 1015 eV.

Cosmic rays may be upwards of a ZeV (1021 eV). Ultra high energy neutrons are around an EeV (1018 eV). But, X-rays only range up to about 120 keV, while the visible (visual) range is around 2 eV.

Astronomy likely started with visual astronomy. Visual refers to that portion of the electromagnetic spectrum called the visible spectrum. Probing the sky with additional portions of this spectrum is difficult as the atmosphere absorbs over many portions.

This has produced fields of observational astronomy based on some portions of the electromagnetic spectrum:

  1. Gamma-ray astronomy,
  2. X-ray astronomy,
  3. Ultraviolet astronomy,
  4. Infrared astronomy, and
  5. Radio astronomy.


The subpage hosts essays and explorations. Some of these may represent nonstandard physics.

Learning groups[edit]

See also[edit]


  1. 1.0 1.1 Philip B. Gove, ed (1963). Webster's Seventh New Collegiate Dictionary. Springfield, Massachusetts: G. & C. Merriam Company. pp. 1221. 
  2. (August 28, 2013) "physics". Wiktionary. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2013-09-30. 
  3. "Compact fluorescent lamp, In: Wikipedia". San Francisco, California: Wikimedia Foundation, Inc. June 10. 2012. Retrieved 2012-06-16. 
  4. 4.0 4.1 4.2 "Standard conditions for temperature and pressure, In: Wikipedia". San Francisco, California: Wikimedia Foundation, Inc. June 16, 2012. Retrieved 2012-06-16. 
  5. 5.0 5.1 Alan D. McNaught, Andrew Wilkinson (1997). Compendium of Chemical Terminology, The Gold Book (2nd ed.). Blackwell Science. ISBN 0-86542-684-8. 
  6. Natural gas – Standard reference conditions (ISO 13443). Geneva, Switzerland: International Organization for Standardization. 1996. 
  7. "line of sight, In: Wiktionary". San Francisco, California: Wikimedia Foundation, Inc. May 3, 2012. Retrieved 2012-06-16. 
  8. 8.0 8.1 8.2 8.3 8.4 Samuel J. Johnson (1874). "Occultations of and by Venus". Astronomical register 12: 268-70. Bibcode1874AReg...12..268J. Retrieved on 2011-11-05. 
  9. (June 16, 2012) "Cartesian coordinate system". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  10. (June 2, 2012) "Distance". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  11. (January 24, 2012) "Emptiness (disambiguation)". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  12. (May 29, 2012) "empty". Wiktionary. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  13. (April 13, 2012) "Empty space". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  14. U. Lindner, J. Einasto, M. Einasto, W. Freudling, K. Fricke, E. Tago (1995). "The Structure of Supervoids I: Void Hierarchy in the Northern Local Supervoid The structure of supervoids. I. Void hierarchy in the Northern Local Supervoid". Astron. Astrophys. 301: 329. Bibcode1995A&A...301..329L. 
  15. (May 2, 2012) "Void (astronomy)". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  16. "Table 3. Coherent derived units in the SI with special names and symbols, In: The International System of Units (SI)". International Bureau of Weights and Measures. 2006. 
  17. - Proposition 75, Theorem 35: p.956 - I.Bernard Cohen and Anne Whitman, translators: Isaac Newton, The Principia: Mathematical Principles of Natural Philosophy. Preceded by A Guide to Newton's Principia, by I.Bernard Cohen. University of California Press 1999 ISBN 0-520-08816-6 ISBN 0-520-08817-4
  18. "CODATA2006". 
  19. (July 12, 2013) "energy". Wiktionary. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2013-07-14. 
  20. (June 20, 2013) "matter". Wiktionary. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2013-07-04. 
  21. (June 15, 2012) "Mass". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  22. (June 14, 2012) "Measurement". Wikipedia. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-06-16. 
  23. 23.0 23.1 23.2 23.3 P. K. Seidelmann (1976). "Measuring the Universe The IAU and astronomical units". The International Astronomical Union. Retrieved 2011-11-27. 
  24. Arora, M. G.; Singh, M. (1994). Nuclear Chemistry. Anmol Publications. p. 202. ISBN 81-261-1763-X. Retrieved 2011-04-02. 
  25. Saha, Gopal (2010). Fundamentals of Nuclear Pharmacy (Sixth ed.). Springer Science+Business Media. p. 11. ISBN 1-4419-5859-2. Retrieved 2011-04-02. 

Further reading[edit]

External links[edit]