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The molar heat capacity is approximately equal to the three timesthe gas constant.
Einstein-Podolsky-Rosen effect

Consider the following quantum mechanical thought-experiment:Take a particle which is at rest and has spin zero. Itspontaneously decays into two fermions (spin 0.5 particles), whichstream away in opposite directions at high speed. Due to the lawof conservation of spin, we know that one is a spin +0.5 and theother is spin -0.5. Which one is which? According to quantummechanics, neither takes on a definite state until it is observed(the wavefunction is collapsed).

The EPR effect demonstrates that if one of the particles isdetected, and its spin is then measured, then the other particle-- no matter where it is in the Universe -- instantaneously isforced to choose as well and take on the role of the otherparticle. This illustrates that certain kinds of quantuminformation travel instantaneously; not everything is limited bythe speed of light.

However, it can be easily demonstrated that this effect doesnot make faster-than-light communication possible.
Equivalence principle

The basic postulate of A. Einstein's general theory of relativity,which posits that an acceleration is fundamentallyindistinguishable from a gravitational field. In other words, ifyou are in an elevator which is utterly sealed and protected fromthe outside, so that you cannot "peek outside," then if you feel aforce (weight), it is fundamentally impossible for you to saywhether the elevator is present in a gravitational field, orwhether the elevator has rockets attached to it and isaccelerating
"upward."

The equivalence principle predicts interesting generalrelativistic effects because not only are the twoindistinguishable to human observers, but also to the Universe aswell, in a way -- any effect that takes place when an observer isaccelerating should also take place in a gravitational field, andvice versa.
Ergosphere

The region around a rotating black hole, between the event horizonand the static limit, where rotational energy can be extractedfrom the black hole.
Event horizon

The radius of surrounding a black hole at which a particle wouldneed an escape velocity of lightspeed to escape; that is, thepoint of no return for a black hole.
Faraday constant; F (M. Faraday)

The electric charge carried by one mole of electrons (or singly-ionized ions). It is equal to the product of the Avogadroconstant and the
(absolute value of the) charge on an electron; itis
9.648670.104 C/mol.
Faraday's law (M. Faraday)

The line integral of the electric flux around a closed curve isproportional to the instantaneous time rate of change of themagnetic flux through a surface bounded by that closed curve.
Faraday's laws of electrolysis (M. Faraday)
1. The amount of chemical change during electrolysis is proportional to the charge passed.

2. The charge required to deposit or liberate a mass is proportional to the charge of the ion, the mass, and inversely proprtional to the relative ionic mass. The constant of proportionality is the Faraday constant.
Faraday's laws of electromagnetic induction (M. Faraday)
1. An electromotive force is induced in a conductor when the magnetic field surrounding it changes.
2. The magnitude of the electromotive force is proportional to the rate of change of the field.

3. The sense of the induced electromotive force depends on the direction of the rate of the change of the field.
Fermat's principle; principle of least time (P. de Fermat)

The principle, put forth by P. de Fermat, states that the pathtaken by a ray of light between any two points in a system isalways the path that takes the least time.
Fermi paradox

E. Fermi's conjecture, simplified with the phrase, "Where arethey?" questioning that if the Galaxy is filled with intelligentand technological civilizations, why haven't they come to us yet?There are several possible answers to this question, but since weonly have the vaguest idea what the right conditions for life andintelligence in our Galaxy, it and Fermi's paradox are no morethan speculation.
Gauss' law (K.F. Gauss)

The electric flux through a closed surface is proportional to thealgebraic sum of electric charges contained within that closedsurface.
Gauss' law for magnetic fields (K.F. Gauss)

The magnetic flux through a closed surface is zero; no magneticcharges exist.
Grandfather paradox

A paradox proposed to discount time travel and show why itviolates causality. Say that your grandfather builds a timemachine. In the present, you use his time machine to go back intime a few decades to a point before he married his wife (yourgrandmother). You meet him to talk about things, and an argumentensues (presumably he doesn't believe that you're hisgrandson/granddaughter), and you accidentally kill him.

If he died before he met your grandmother and never hadchildren, then your parents could certainly never have met (one ofthem didn't exist!) and could never have given birth to you. Inaddition, if he didn't live to build his time machine, what areyou doing here in the past alive and with a time machine, if youwere never born and it was never built?
Hall effect

When charged particles flow through a tube which has both anelectric field and a magnetic field (perpendicular to the electricfield) present in it, only certain velocities of the chargedparticles are preferred, and will make it undeviated through thetube; the rest will be deflected into the sides. This effect isexploited in such devices as the mass spectrometer and in theThompson experiment. This is called the Hall effect.
Hawking radiation (S.W. Hawking; 1973)

The theory that black holes emit radiation like any other hotbody.
Virtual particle-antiparticle pairs are constantly beingcreated in supposedly empty space. Every once in a while, onewill be created in the vicinity of a black hole's event horizon.One of these particles might be catpured by the black hole,forever trapped, while the other might escape the black hole'sgravity. The trapped particle, which would have negative energy(by definition), would reduce the mass of the black hole, and theparticle which escaped would have positive energy. Thus, from adistant, one would see the black hole's mass decrease and aparticle escape the vicinity; it would appear as if the black holewere emitting radiation. The rate of emission has a negativerelationship with the mass of the black hole; massive black holesemit radiation relatively slowly, while smaller black holes emitradiation -- and thus decrease their mass -- more rapidly.

Heisenberg uncertainty principle (W. Heisenberg; 1927)

A principle, central to quantum mechanics, which states that themomentum (mass times velocity) and the position of a particlecannot both be known to infinite accuracy; the more you know aboutone, the lest you know about the other.

It can be illustrated in a fairly clear way as follows: Tosee something (let's say an electron), we have to fire photons atit, so they bounce off and come back to us, so we can "see" it.If you choose low- frequency photons, with a low energy, they donot impart much momentum to the electron, but they give you a veryfuzzy picture, so you have a higher uncertainty in position sothat you can have a higher certainty in momentum.
On the otherhand, if you were to fire very high-energy photons (x-rays orgammas) at the electron, they would give you a very clear pictureof where the electron is (high certainty in position), but wouldimpart a great deal of momentum to the electron (higheruncertainty in momentum). In a more generalized sense, the uncertainty principle tellsus that the act of observing changes the observed in fundamentalway.
Hooke's law (R. Hooke)

The stress applied to any solid is proportional to the strain itproduces within the elastic limit for that solid. The constant ofthat proportionality is the Young modulus of elasticity for thatsubstance.
Hubble constant; H0 (E.P. Hubble; 1925)

The constant which determines the relationship between thedistance to a galaxy and its velocity of recession due to theexpansion of the Universe.
It is not known to great accuracy, butis believed to lie between 49 and 95
Hubble's law (E.P. Hubble; 1925)

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