Career Employer

Your FREE GRE Physics Flashcards 2026 – 200+ Cards

Realistic GRE Physics flashcards across all nine ETS content areas — flip, match, type, and quiz yourself on the key laws, equations, and constants.

How well do you know them?

To find us again, just search “Career Employer GRE Physics”

By

Click Study Flashcards above to open the flashcard hub — 200 GRE Physics cards you can flip, match, type, or quiz yourself on. Every card is drawn from the ETS content areas, so you study exactly what the test measures.[1] Pair them with our free practice test and study guide.

GRE Physics Flashcard Study Modes

Four modes run on the same deck. Flip is plain study, front to back, at your own pace. Match is a timed term-to-definition game that rewards fast recognition. Type shows the definition and asks you to produce the term, so a card like Brewster’s angle has to come from memory, not from a list. Quiz turns the cards into multiple choice for a quick check.

Free GRE Physics flashcards from Career Employer — active recall for the GRE Physics Subject Test

Why Flashcards Work for the GRE Physics Test

Classical Mechanics is the largest domain at 40 cards, and it drills the vocabulary and relations that show up everywhere else on the GRE Physics test. You get core quantities such as Torque and Momentum alongside the formalism cards, including Lagrangian and Hamiltonian, plus staples like Hooke’s law and Escape velocity that you should be able to state without hesitation.

Electromagnetism follows with 35 cards built around the named laws and the definitions that hang off them. Gauss’s law, Ampere’s law, and Lenz’s law sit next to Coulomb’s law and the Lorentz force, with supporting terms like Magnetic flux and Ohm’s law filling in the circuit and field language you need to read a problem quickly.

Thermodynamics & Statistical Mechanics carries 23 cards covering process types and constants, from Adiabatic process and Isothermal process to Carnot efficiency and the Equipartition theorem. Atomic Physics adds 21 cards on spectra and structure, where the Zeeman effect, the Stark effect, and Hund’s rule appear beside the Rydberg formula and Work function.

Optics & Wave Phenomena has 20 cards on propagation and interference, including Snell’s law, Malus’s law, and Total internal reflection. Quantum Mechanics also has 20, drilling operators and results such as the Momentum operator, the Canonical commutator, and de Broglie wavelength.

The remaining three domains reward cheap points. Laboratory Methods holds 16 cards on instruments like the Lock-in amplifier and the Photomultiplier tube. Special Relativity has 15, covering Proper time, Length contraction, and the Lorentz factor. Specialized Topics closes with 10, including Superconductivity and the Chandrasekhar limit.

The GRE Physics Subject Test rewards instant recall of laws, equations, and constants across nine areas under tight time pressure.[2] Spaced flashcards are the most efficient way to make that knowledge automatic. Used alongside our practice test and study guide, they turn review time into measurable progress.

GRE Physics Flashcards by Area

The cards are organized by the GRE Physics test’s nine ETS content areas. Drill the highest-weighted ones first — Classical Mechanics and Electromagnetism anchor the test at about 38% combined:[1]

GRE Physics flashcards by content area and approximate weighting
Content areaApprox. weight
Classical Mechanics~20%
Electromagnetism~18%
Quantum Mechanics~12%
Atomic Physics~10%
Thermodynamics & Statistical Mechanics~10%
Optics & Wave Phenomena~9%
Specialized Topics (nuclear, particle, condensed matter, astrophysics)~9%
Special Relativity~6%
Laboratory Methods~6%

How to Get the Most Out of These Flashcards

  • Start heavy. Classical Mechanics is 40 cards and feeds every other domain, so clear it in Flip first, then move to the 35 Electromagnetism cards while the definitions are fresh.
  • Type the formalism. Cards like Lagrangian and Canonical commutator are easy to recognize and hard to reproduce, so drill them in Type until the wording comes out cleanly.
  • Match the named laws. The law cards across Electromagnetism and Optics & Wave Phenomena, such as Lenz’s law and Malus’s law, are ideal for timed recognition under Match.
  • Switch when Quiz stops teaching. Once Quiz rounds run clean across Special Relativity and Thermodynamics & Statistical Mechanics, move to the practice test and let the study guide fill the gaps.
  • Keep a rotating cadence. Work one or two domains a sitting, then re-Match yesterday’s set, so the 200 cards cycle through review instead of getting studied once and dropped.

GRE Physics Flashcards FAQ

Two hundred free GRE Physics flashcards, organized across all nine ETS content areas — Classical Mechanics, Electromagnetism, Optics and Wave Phenomena, Thermodynamics and Statistical Mechanics, Quantum Mechanics, Atomic Physics, Special Relativity, Laboratory Methods, and Specialized Topics. They're free with no account required.

GRE Physics flashcard bank

All 200 cards, by topic

A reference copy of every card in this deck. Each answer stays hidden until you choose to show it. To study with Flip, Match, Type and Quiz modes and track what you have mastered, use Study Flashcards at the top of the page.

Classical Mechanics (40)

Newton's second law
Show answer

F⃗=ma⃗ \vec F = m\vec a — net force equals mass times acceleration (more generally F⃗=dp⃗/dt \vec F = d\vec p/dt ).

Work-energy theorem
Show answer

Net work equals the change in kinetic energy: Wnet=ΔKE=12mvf2−12mvi2 W_{net} = \Delta KE = \tfrac{1}{2}mv_f^2 - \tfrac{1}{2}mv_i^2 .

Kinetic energy
Show answer

KE=12mv2 KE = \tfrac{1}{2}mv^2 .

Gravitational potential energy (near Earth)
Show answer

U=mgh U = mgh .

Momentum
Show answer

p⃗=mv⃗ \vec p = m\vec v ; conserved when no net external force acts.

Impulse-momentum theorem
Show answer

J⃗=∫F⃗ dt=Δp⃗ \vec J = \int \vec F\,dt = \Delta \vec p — impulse equals change in momentum.

Elastic collision (equal masses, one at rest)
Show answer

The velocities are exchanged: the incoming mass stops and the struck mass moves off at the original speed.

Perfectly inelastic collision
Show answer

Objects stick together; momentum is conserved (they move at the center-of-mass velocity) but kinetic energy is not.

Centripetal acceleration
Show answer

ac=v2r a_c = \dfrac{v^2}{r} , directed toward the center of the circular path.

Centripetal force
Show answer

Fc=mv2r=mω2r F_c = \dfrac{mv^2}{r} = m\omega^2 r , pointing toward the center.

Acceleration on a frictionless incline (angle θ)
Show answer

a=gsin⁡θ a = g\sin\theta down the slope.

Hooke's law
Show answer

F=−kx F = -kx — the restoring force of an ideal spring, proportional to displacement.

Angular frequency of a mass-spring system
Show answer

ω=km \omega = \sqrt{\dfrac{k}{m}} .

Period of a simple pendulum
Show answer

T=2πLg T = 2\pi\sqrt{\dfrac{L}{g}} (small oscillations).

Simple harmonic motion
Show answer

Motion under a restoring force proportional to displacement: x(t)=Acos⁡(ωt+ϕ) x(t) = A\cos(\omega t + \phi) .

Torque
Show answer

τ⃗=r⃗×F⃗ \vec\tau = \vec r\times\vec F ; the rotational analog of force, with τ=Iα \tau = I\alpha .

Moment of inertia
Show answer

I=∑miri2 I = \sum m_i r_i^2 (or ∫r2 dm \int r^2\,dm ) — rotational analog of mass.

Parallel-axis theorem
Show answer

I=Icm+Md2 I = I_{cm} + Md^2 , where d d is the distance from the center-of-mass axis to the parallel axis.

Moment of inertia of a thin rod about its end
Show answer

I=13ML2 I = \tfrac{1}{3}ML^2 (about its center it is 112ML2 \tfrac{1}{12}ML^2 ).

Moment of inertia of a solid sphere (center)
Show answer

I=25MR2 I = \tfrac{2}{5}MR^2 ; about a tangent axis it is 75MR2 \tfrac{7}{5}MR^2 .

Angular momentum
Show answer

L⃗=Iω⃗ \vec L = I\vec\omega (or r⃗×p⃗ \vec r\times\vec p ); conserved when no external torque acts.

Rotational kinetic energy
Show answer

KErot=12Iω2 KE_{rot} = \tfrac{1}{2}I\omega^2 .

Why a spinning skater speeds up pulling in her arms
Show answer

Conservation of angular momentum Iω= I\omega = constant — reducing I I raises ω \omega ; her rotational KE increases (work done pulling in).

Newton's law of universal gravitation
Show answer

F=Gm1m2r2 F = \dfrac{Gm_1 m_2}{r^2} .

Escape velocity
Show answer

vesc=2GMR v_{esc} = \sqrt{\dfrac{2GM}{R}} ; independent of the escaping object's mass, 2× \sqrt{2}\times the surface orbital speed.

Kepler's third law
Show answer

T2∝a3 T^2 \propto a^3 — the square of the orbital period is proportional to the cube of the semi-major axis.

Kepler's second law
Show answer

A planet sweeps equal areas in equal times — a consequence of angular-momentum conservation; it moves fastest at perihelion.

Lagrangian
Show answer

L=T−V L = T - V (kinetic minus potential energy) in generalized coordinates.

Euler-Lagrange equation
Show answer

ddt∂L∂q˙−∂L∂q=0 \dfrac{d}{dt}\dfrac{\partial L}{\partial \dot q} - \dfrac{\partial L}{\partial q} = 0 for each generalized coordinate.

Hamiltonian
Show answer

H=T+V H = T + V — total energy in coordinates and momenta; Hamilton's equations q˙=∂H/∂p, p˙=−∂H/∂q \dot q = \partial H/\partial p,\ \dot p = -\partial H/\partial q .

Generalized (canonical) momentum
Show answer

pi=∂L∂q˙i p_i = \dfrac{\partial L}{\partial \dot q_i} — conserved if L L does not depend on qi q_i (a cyclic coordinate).

Coriolis acceleration
Show answer

a⃗Cor=−2 ω⃗×v⃗ \vec a_{Cor} = -2\,\vec\omega\times\vec v in a rotating frame; deflects motion to the right in the Northern Hemisphere.

Centrifugal acceleration (rotating frame)
Show answer

−ω⃗×(ω⃗×r⃗) -\vec\omega\times(\vec\omega\times\vec r) , pointing outward; magnitude ω2r \omega^2 r .

Tsiolkovsky rocket equation
Show answer

Δv=veln⁡ ⁣mimf \Delta v = v_e \ln\!\dfrac{m_i}{m_f} — change in speed from exhaust speed and the initial-to-final mass ratio.

Reduced mass (two-body problem)
Show answer

μ=m1m2m1+m2 \mu = \dfrac{m_1 m_2}{m_1 + m_2} — converts a two-body problem into an equivalent one-body problem.

Period of a physical pendulum
Show answer

T=2πImgd T = 2\pi\sqrt{\dfrac{I}{mgd}} , where d d is the pivot-to-center-of-mass distance.

Power
Show answer

P=dWdt=F⃗⋅v⃗ P = \dfrac{dW}{dt} = \vec F\cdot\vec v .

Conservative force
Show answer

A force whose work is path-independent and equals minus a potential-energy change; F⃗=−∇U \vec F = -\nabla U .

Friction force (kinetic)
Show answer

fk=μkN f_k = \mu_k N , opposing motion; static friction satisfies fs≤μsN f_s \le \mu_s N .

Terminal velocity
Show answer

The constant speed where drag balances gravity, so net force and acceleration are zero.

Electromagnetism (35)

Coulomb's law
Show answer

F=14πε0q1q2r2 F = \dfrac{1}{4\pi\varepsilon_0}\dfrac{q_1 q_2}{r^2} — force between two point charges.

Electric field of a point charge
Show answer

E=14πε0qr2 E = \dfrac{1}{4\pi\varepsilon_0}\dfrac{q}{r^2} , directed radially.

Gauss's law
Show answer

∮E⃗⋅dA⃗=Qencε0 \oint \vec E\cdot d\vec A = \dfrac{Q_{enc}}{\varepsilon_0} — electric flux through a closed surface equals enclosed charge over ε0 \varepsilon_0 .

Electric field inside a conductor (electrostatic equilibrium)
Show answer

Zero; any excess charge resides on the conductor's surface.

Electric potential energy / potential
Show answer

U=14πε0q1q2r U = \dfrac{1}{4\pi\varepsilon_0}\dfrac{q_1 q_2}{r} ; potential of a point charge V=14πε0qr V = \dfrac{1}{4\pi\varepsilon_0}\dfrac{q}{r} .

Relation between E and V
Show answer

E⃗=−∇V \vec E = -\nabla V — the field points down the steepest decrease of potential.

Capacitance of a parallel-plate capacitor
Show answer

C=κε0Ad C = \dfrac{\kappa\varepsilon_0 A}{d} ; inserting a dielectric κ \kappa raises the capacitance.

Energy stored in a capacitor
Show answer

U=12CV2=Q22C=12QV U = \tfrac{1}{2}CV^2 = \dfrac{Q^2}{2C} = \tfrac{1}{2}QV .

Ohm's law
Show answer

V=IR V = IR .

Power dissipated in a resistor
Show answer

P=IV=I2R=V2R P = IV = I^2 R = \dfrac{V^2}{R} .

Resistors in series vs parallel
Show answer

Series: R=R1+R2+… R = R_1 + R_2 + \dots . Parallel: 1R=1R1+1R2+… \dfrac{1}{R} = \dfrac{1}{R_1} + \dfrac{1}{R_2} + \dots .

Capacitors in series vs parallel
Show answer

Parallel: C=C1+C2+… C = C_1 + C_2 + \dots . Series: 1C=1C1+1C2+… \dfrac{1}{C} = \dfrac{1}{C_1} + \dfrac{1}{C_2} + \dots (opposite of resistors).

RC time constant
Show answer

τ=RC \tau = RC — charge on the capacitor relaxes as e−t/τ e^{-t/\tau} .

RL time constant
Show answer

τ=LR \tau = \dfrac{L}{R} .

Kirchhoff's rules
Show answer

Junction rule: currents into a node sum to zero (charge conservation). Loop rule: voltages around a closed loop sum to zero (energy conservation).

Lorentz force
Show answer

F⃗=qE⃗+qv⃗×B⃗ \vec F = q\vec E + q\vec v\times\vec B — force on a charge from electric and magnetic fields.

Magnetic field of a long solenoid
Show answer

B=μ0nI B = \mu_0 n I , where n n is turns per unit length.

Ampere's law
Show answer

∮B⃗⋅dl⃗=μ0Ienc \oint \vec B\cdot d\vec l = \mu_0 I_{enc} — gives B from current with high symmetry.

Biot-Savart law
Show answer

dB⃗=μ04πI dl⃗×r^r2 d\vec B = \dfrac{\mu_0}{4\pi}\dfrac{I\,d\vec l\times\hat r}{r^2} — field from a current element.

Force between parallel currents
Show answer

Attractive when the currents are in the same direction, repulsive when opposite.

Faraday's law of induction
Show answer

ε=−dΦBdt \varepsilon = -\dfrac{d\Phi_B}{dt} — a changing magnetic flux induces an EMF.

Lenz's law
Show answer

The induced current flows so as to oppose the change in magnetic flux that produced it (the minus sign in Faraday's law).

Self-inductance of a solenoid
Show answer

Proportional to the square of the number of turns, L∝N2 L \propto N^2 (also to area and core permeability).

Energy stored in an inductor
Show answer

U=12LI2 U = \tfrac{1}{2}LI^2 .

SI unit of magnetic flux
Show answer

The weber (Wb); 1 Wb=1 T⋅m2 1\ \text{Wb} = 1\ \text{T}\cdot\text{m}^2 .

Maxwell's equations
Show answer

Gauss's law, Gauss's law for magnetism (∇⋅B⃗=0 \nabla\cdot\vec B = 0 ), Faraday's law, and the Ampere-Maxwell law — the four laws of electromagnetism.

Speed of an EM wave in vacuum
Show answer

c=1μ0ε0≈3.0×108 c = \dfrac{1}{\sqrt{\mu_0\varepsilon_0}} \approx 3.0\times10^8 m/s.

Properties of electromagnetic waves
Show answer

Transverse, require no medium, travel at c c in vacuum, consist of oscillating E⃗ \vec E and B⃗ \vec B fields perpendicular to each other and to the motion.

Poynting vector
Show answer

S⃗=1μ0E⃗×B⃗ \vec S = \dfrac{1}{\mu_0}\vec E\times\vec B — energy flux (power per area) carried by an EM field.

Capacitive reactance
Show answer

XC=1ωC X_C = \dfrac{1}{\omega C} ; in a capacitor, current leads voltage by 90°.

Inductive reactance
Show answer

XL=ωL X_L = \omega L ; in an inductor, current lags voltage by 90°.

Resonance in an LC / RLC circuit
Show answer

ω0=1LC \omega_0 = \dfrac{1}{\sqrt{LC}} — where XL=XC X_L = X_C and the impedance is minimized.

Magnetic flux
Show answer

ΦB=∫B⃗⋅dA⃗ \Phi_B = \int \vec B\cdot d\vec A — the field component through a surface times its area.

Cyclotron frequency
Show answer

ω=qBm \omega = \dfrac{qB}{m} — angular frequency of a charge circling in a magnetic field.

Principle of superposition (fields)
Show answer

The net electric (or magnetic) field at a point is the vector sum of the fields from each source.

Optics & Wave Phenomena (20)

Wave speed relation
Show answer

v=λf v = \lambda f — speed equals wavelength times frequency.

What stays constant when a wave changes medium?
Show answer

The frequency. The wavelength and speed change, but the frequency is fixed by the source.

Snell's law
Show answer

n1sin⁡θ1=n2sin⁡θ2 n_1\sin\theta_1 = n_2\sin\theta_2 — governs refraction at an interface.

Index of refraction
Show answer

n=cv n = \dfrac{c}{v} ; light slows (v v decreases) in a higher-index medium.

Total internal reflection
Show answer

Occurs when light in a denser medium hits the boundary beyond the critical angle θc=sin⁡−1(n2/n1) \theta_c = \sin^{-1}(n_2/n_1) ; confines light in optical fibers.

Thin-lens / mirror equation
Show answer

1f=1do+1di \dfrac{1}{f} = \dfrac{1}{d_o} + \dfrac{1}{d_i} ; magnification m=−dido m = -\dfrac{d_i}{d_o} .

Double-slit bright fringes
Show answer

dsin⁡θ=mλ d\sin\theta = m\lambda — constructive interference at integer path differences.

Single-slit diffraction minima
Show answer

asin⁡θ=mλ a\sin\theta = m\lambda (m=±1,±2,… m = \pm1, \pm2, \dots ) — dark fringes for a slit of width a a .

Double-slit fringe spacing
Show answer

Proportional to the wavelength and inversely proportional to the slit separation: Δy=λLd \Delta y = \dfrac{\lambda L}{d} .

Brewster's angle
Show answer

θB=tan⁡−1(n) \theta_B = \tan^{-1}(n) — the incidence angle at which reflected light is fully polarized.

Malus's law
Show answer

I=I0cos⁡2θ I = I_0\cos^2\theta — intensity of polarized light through a polarizer at angle θ \theta .

Unpolarized light through a polarizer
Show answer

Exactly half the intensity, 12I0 \tfrac{1}{2}I_0 , is transmitted (and the output is polarized).

Doppler effect (light)
Show answer

Approaching source → blueshift (higher frequency); receding source → redshift (lower frequency).

Interference vs diffraction
Show answer

Interference = superposition of waves from multiple sources; diffraction = bending/spreading of a single wave around edges or apertures.

Which phenomenon needs the particle theory of light?
Show answer

The photoelectric effect. Interference, diffraction, and polarization are all explained by the wave theory.

Diffraction-grating maxima
Show answer

dsin⁡θ=mλ d\sin\theta = m\lambda ; a grating gives sharp, widely separated orders for spectroscopy.

Rayleigh criterion (resolution)
Show answer

θ≈1.22λD \theta \approx 1.22\dfrac{\lambda}{D} — minimum angular separation a circular aperture of diameter D D can resolve.

Standing wave on a string fixed at both ends
Show answer

λn=2Ln, fn=nv2L \lambda_n = \dfrac{2L}{n},\ f_n = \dfrac{nv}{2L} — harmonics for n=1,2,3,… n = 1, 2, 3, \dots .

Color with the shortest visible wavelength
Show answer

Violet (refracted/dispersed most by a prism); red has the longest visible wavelength.

Why does a prism disperse light?
Show answer

The index of refraction depends on wavelength (dispersion), so different colors bend by different amounts.

Thermodynamics & Statistical Mechanics (23)

First law of thermodynamics
Show answer

ΔU=Q−W \Delta U = Q - W — change in internal energy equals heat added minus work done by the system.

Second law of thermodynamics
Show answer

The entropy of an isolated system never decreases; heat does not spontaneously flow from cold to hot.

Third law of thermodynamics
Show answer

The entropy of a perfect crystal approaches zero as the temperature approaches absolute zero.

Ideal gas law
Show answer

PV=nRT PV = nRT (or PV=NkBT PV = Nk_B T ).

Isothermal process
Show answer

T T constant, so ΔU=0 \Delta U = 0 and Q=W Q = W for an ideal gas.

Isobaric process
Show answer

P P constant; work done by the gas is W=P ΔV W = P\,\Delta V .

Isochoric (isovolumetric) process
Show answer

V V constant, so W=0 W = 0 and Q=ΔU Q = \Delta U .

Adiabatic process
Show answer

No heat exchange, Q=0 Q = 0 , so ΔU=−W \Delta U = -W ; for an ideal gas PVγ= PV^\gamma = constant.

Adiabatic free expansion (ideal gas)
Show answer

No work and no heat, so ΔU=0 \Delta U = 0 ; since U U depends only on T T , the temperature stays constant.

Carnot efficiency
Show answer

η=1−TcTh \eta = 1 - \dfrac{T_c}{T_h} (kelvin) — the maximum efficiency of any engine between two reservoirs.

Entropy change (reversible)
Show answer

dS=dQrevT dS = \dfrac{dQ_{rev}}{T} ; for a reversible cycle the total entropy change of the universe is zero.

Boltzmann entropy formula
Show answer

S=kBln⁡Ω S = k_B \ln \Omega — entropy in terms of the number of accessible microstates Ω \Omega .

Equipartition theorem
Show answer

Each quadratic degree of freedom contributes 12kBT \tfrac{1}{2}k_B T to the average energy.

Average translational kinetic energy of a gas molecule
Show answer

⟨KE⟩=32kBT \langle KE\rangle = \tfrac{3}{2}k_B T — independent of molecular mass.

RMS speed of gas molecules
Show answer

vrms=3kBTm v_{rms} = \sqrt{\dfrac{3k_B T}{m}} — heavier molecules move slower at the same temperature.

Maxwell-Boltzmann distribution
Show answer

The classical distribution of molecular speeds in an ideal gas; raising T T broadens it and shifts the peak to higher speed.

Stefan-Boltzmann law
Show answer

P=σAT4 P = \sigma A T^4 — total power radiated by a blackbody is proportional to T4 T^4 .

Wien's displacement law
Show answer

λmaxT= \lambda_{max} T = constant — a hotter blackbody peaks at a shorter wavelength.

Boltzmann constant
Show answer

kB≈1.38×10−23 k_B \approx 1.38\times10^{-23} J/K — links temperature to energy (kB=R/NA k_B = R/N_A ).

Heat capacity / specific heat
Show answer

Q=mc ΔT Q = mc\,\Delta T ; for a gas, CP−CV=R C_P - C_V = R per mole (Mayer's relation).

Heat pump / refrigerator
Show answer

Moves heat from cold to hot using external work — a consequence (and demonstration) of the second law.

Fermi-Dirac vs Bose-Einstein statistics
Show answer

Fermi-Dirac governs fermions (one per state, Pauli); Bose-Einstein governs bosons (many can share a state).

Internal energy of an ideal gas
Show answer

Depends only on temperature; for a monatomic ideal gas U=32nRT U = \tfrac{3}{2}nRT .

Quantum Mechanics (20)

Schrodinger equation (time-independent)
Show answer

H^ψ=Eψ \hat H\psi = E\psi — gives the stationary states ψ \psi and their energies E E .

Schrodinger equation (time-dependent)
Show answer

iℏ∂ψ∂t=H^ψ i\hbar\dfrac{\partial \psi}{\partial t} = \hat H\psi .

Born rule (probability density)
Show answer

∣ψ(x)∣2 |\psi(x)|^2 is the probability density; the probability in [a,b] [a,b] is ∫ab∣ψ∣2 dx \int_a^b |\psi|^2\,dx .

Normalization condition
Show answer

∫−∞∞∣ψ∣2 dx=1 \int_{-\infty}^{\infty} |\psi|^2\,dx = 1 — total probability is one.

Infinite square well energies
Show answer

En=n2h28mL2=n2π2ℏ22mL2 E_n = \dfrac{n^2 h^2}{8mL^2} = \dfrac{n^2\pi^2\hbar^2}{2mL^2} , n=1,2,3,… n = 1, 2, 3, \dots

Infinite square well wave functions
Show answer

ψn(x)=2Lsin⁡ ⁣(nπxL) \psi_n(x) = \sqrt{\dfrac{2}{L}}\sin\!\left(\dfrac{n\pi x}{L}\right) .

Quantum harmonic oscillator energies
Show answer

En=(n+12)ℏω E_n = \left(n + \tfrac{1}{2}\right)\hbar\omega — evenly spaced levels with zero-point energy 12ℏω \tfrac{1}{2}\hbar\omega .

Canonical commutator
Show answer

[x^,p^]=iℏ [\hat x,\hat p] = i\hbar — position and momentum operators do not commute.

Heisenberg uncertainty principle
Show answer

Δx Δp≥ℏ2 \Delta x\,\Delta p \ge \dfrac{\hbar}{2} ; an energy-time form is ΔE Δt≥ℏ2 \Delta E\,\Delta t \ge \dfrac{\hbar}{2} .

Hamiltonian operator
Show answer

H^ \hat H represents the total energy of the system; its eigenvalues are the allowed energies.

Momentum operator
Show answer

p^=−iℏ∂∂x \hat p = -i\hbar\dfrac{\partial}{\partial x} .

Orthonormality of eigenstates
Show answer

Energy eigenstates are orthogonal and normalized: ∫ψm∗ψn dx=δmn \int \psi_m^* \psi_n\,dx = \delta_{mn} .

Expectation value
Show answer

⟨A⟩=∫ψ∗A^ ψ dx \langle A\rangle = \int \psi^* \hat A\,\psi\,dx — the average measured value of observable A^ \hat A .

Quantum tunneling
Show answer

A particle has a nonzero probability of passing through a potential barrier even when its energy is below the barrier height.

Electron spin quantum number
Show answer

s=12 s = \tfrac{1}{2} ; the electron is a spin-½ fermion with two spin projections ms=±12 m_s = \pm\tfrac{1}{2} .

Pauli exclusion principle
Show answer

No two identical fermions can occupy the same quantum state simultaneously.

de Broglie wavelength
Show answer

λ=hp \lambda = \dfrac{h}{p} — every particle has a wave nature, demonstrated by electron diffraction.

Ehrenfest's theorem
Show answer

Quantum expectation values obey the classical equations of motion (m d⟨x⟩/dt=⟨p⟩ m\,d\langle x\rangle/dt = \langle p\rangle ).

Eigenvalue equation
Show answer

A^ψ=aψ \hat A\psi = a\psi : a measurement of A^ \hat A on eigenstate ψ \psi yields the eigenvalue a a with certainty.

Angular-momentum quantization
Show answer

L2=l(l+1)ℏ2 L^2 = l(l+1)\hbar^2 and Lz=mlℏ L_z = m_l\hbar — magnitude and projection are both quantized.

Atomic Physics (21)

Bohr model energy levels (hydrogen)
Show answer

En=−13.6 eVn2 E_n = -\dfrac{13.6\,\text{eV}}{n^2} ; the ground state is −13.6 -13.6 eV.

Bohr quantization of angular momentum
Show answer

L=nℏ L = n\hbar — orbital angular momentum is an integer multiple of ℏ \hbar .

Photon energy
Show answer

E=hf=hcλ E = hf = \dfrac{hc}{\lambda} ; emitted photon energy equals the gap between two atomic levels.

Rydberg formula
Show answer

1λ=R(1n12−1n22) \dfrac{1}{\lambda} = R\left(\dfrac{1}{n_1^2} - \dfrac{1}{n_2^2}\right) — wavelengths of hydrogen spectral lines.

Lyman, Balmer, Paschen series
Show answer

Transitions ending at n=1 n = 1 (Lyman, UV), n=2 n = 2 (Balmer, visible), n=3 n = 3 (Paschen, IR).

Longest-wavelength visible hydrogen line
Show answer

The n=3→2 n = 3 \to 2 Balmer transition (H-alpha) — the smallest energy gap gives the longest wavelength.

Four atomic quantum numbers
Show answer

Principal n n , azimuthal l l , magnetic ml m_l , and spin ms m_s — they label every electron state.

Photoelectric effect
Show answer

KEmax=hf−ϕ KE_{max} = hf - \phi ; below a threshold frequency no electrons are emitted, evidence for photons.

Work function
Show answer

ϕ \phi , the minimum energy to free an electron from a metal surface.

Fine structure
Show answer

Small spectral-line splitting from spin-orbit coupling — the electron's spin interacting with its orbital motion.

Hyperfine structure
Show answer

Even smaller splitting from the interaction between the nuclear spin and the electron cloud.

Zeeman effect
Show answer

Splitting of atomic energy levels (and spectral lines) in an external magnetic field.

Stark effect
Show answer

Shifting and splitting of spectral lines in an external electric field (the electric analog of the Zeeman effect).

Stern-Gerlach experiment
Show answer

An atomic beam splits into discrete components in a non-uniform magnetic field — proof that angular momentum (spin) is quantized.

Compton scattering
Show answer

Δλ=hmec(1−cos⁡θ) \Delta\lambda = \dfrac{h}{m_e c}(1-\cos\theta) — wavelength shift of an X-ray photon scattering off an electron; evidence for photon momentum.

Electron diffraction (Davisson-Germer)
Show answer

Electrons form interference patterns, demonstrating their wave nature (wave-particle duality).

Hund's rule
Show answer

Electrons fill degenerate orbitals singly with parallel spins before pairing, to minimize energy.

Aufbau principle
Show answer

Electrons fill the lowest-energy orbitals first when building up an atom's ground-state configuration.

Selection rule for dipole transitions
Show answer

Δl=±1 \Delta l = \pm1 (and Δml=0,±1 \Delta m_l = 0, \pm1 ) — allowed electric-dipole transitions.

X-ray production (characteristic lines)
Show answer

An inner-shell vacancy filled by an outer electron emits a characteristic X-ray; K-alpha is n=2→1 n=2 \to 1 .

What keeps the electron from falling into the nucleus?
Show answer

The uncertainty principle: confining the electron more tightly raises its momentum (and energy), setting a minimum-energy ground state.

Special Relativity (15)

Two postulates of special relativity
Show answer

(1) The laws of physics are the same in all inertial frames. (2) The speed of light c c is the same for every observer.

Lorentz factor
Show answer

γ=11−v2/c2 \gamma = \dfrac{1}{\sqrt{1 - v^2/c^2}} — scales time dilation, length contraction, and energy.

Time dilation
Show answer

Δt=γ Δt0 \Delta t = \gamma\,\Delta t_0 — a moving clock runs slow; Δt0 \Delta t_0 is the proper time in the clock's rest frame.

Length contraction
Show answer

L=L0γ L = \dfrac{L_0}{\gamma} — a moving object is shortened along its direction of motion; L0 L_0 is the proper length.

Proper time
Show answer

The time interval measured by a clock at rest relative to the two events — the shortest possible interval between them.

Lorentz transformation
Show answer

x′=γ(x−vt), t′=γ ⁣(t−vxc2) x' = \gamma(x - vt),\ t' = \gamma\!\left(t - \dfrac{vx}{c^2}\right) — relates coordinates between inertial frames.

Relativistic energy
Show answer

E=γmc2 E = \gamma mc^2 ; rest energy is E0=mc2 E_0 = mc^2 .

Relativistic momentum
Show answer

p⃗=γmv⃗ \vec p = \gamma m\vec v .

Energy-momentum relation
Show answer

E2=(pc)2+(mc2)2 E^2 = (pc)^2 + (mc^2)^2 ; for a photon E=pc E = pc , at rest E=mc2 E = mc^2 .

Relativistic kinetic energy
Show answer

KE=(γ−1)mc2 KE = (\gamma - 1)mc^2 — reduces to 12mv2 \tfrac{1}{2}mv^2 at low speed and grows without bound as v→c v\to c .

Relativistic velocity addition
Show answer

u′=u+v1+uv/c2 u' = \dfrac{u + v}{1 + uv/c^2} — keeps the result below c c .

Invariant spacetime interval
Show answer

Δs2=(cΔt)2−Δx2 \Delta s^2 = (c\Delta t)^2 - \Delta x^2 — the same for all inertial observers.

Relativistic Doppler effect
Show answer

Includes time dilation, so it differs from the classical Doppler shift; receding source → redshift, approaching → blueshift.

Twin paradox resolution
Show answer

The traveling twin accelerates and decelerates, breaking the symmetry, so that twin ages less.

Why can't a massive object reach c?
Show answer

Its kinetic energy (γ−1)mc2 (\gamma-1)mc^2 diverges as v→c v\to c — infinite energy would be required.

Laboratory Methods (16)

Random vs systematic error
Show answer

Random error scatters measurements (reduced by averaging); systematic error biases them in one direction (a calibration/offset problem).

Adding independent uncertainties
Show answer

They add in quadrature: σ=σ12+σ22 \sigma = \sqrt{\sigma_1^2 + \sigma_2^2} .

Poisson counting statistics
Show answer

A count of N N events has uncertainty N \sqrt{N} ; the fractional uncertainty 1/N 1/\sqrt{N} shrinks with more data.

Standard deviation vs standard error
Show answer

Standard deviation measures spread; the standard error of the mean is σ/N \sigma/\sqrt{N} .

Lock-in amplifier
Show answer

Extracts a small signal at a known reference frequency from heavy noise, by mixing and low-pass filtering, hugely improving signal-to-noise.

Faraday cage
Show answer

A conducting enclosure that shields its contents from external electric fields (charges redistribute to cancel the field inside).

Cryostat with liquid helium
Show answer

Provides thermal insulation to reach and hold temperatures near absolute zero; liquid helium boils at 4.2 K.

Laser (Doppler) cooling
Show answer

Slows and cools atoms using laser light tuned just below an atomic transition, reducing their kinetic energy.

Optical tweezers
Show answer

Trap and move microscopic particles using the radiation pressure (momentum) of a focused laser beam.

Hall effect measurement
Show answer

Measures the carrier density (and sign of charge carriers) in a material from the transverse Hall voltage in a magnetic field.

Time-of-flight mass spectrometry
Show answer

Determines an ion's mass-to-charge ratio from the time it takes to travel a known distance after acceleration.

FTIR spectroscopy advantage
Show answer

Fourier-transform IR offers higher resolution, faster acquisition, and better signal-to-noise (Fellgett's advantage) over dispersive IR.

Oscilloscope
Show answer

Displays voltage versus time, used to view waveforms, measure amplitude, frequency, and phase.

Significant figures rule
Show answer

A computed result is limited by the least-precise input; report uncertainty to one or two significant figures.

Photomultiplier tube
Show answer

Detects single photons by cascading secondary-electron emission, producing a measurable pulse from very weak light.

Geiger-Muller counter
Show answer

Detects ionizing radiation via gas ionization producing electrical pulses; counts follow Poisson statistics.

Specialized Topics (10)

Nuclear magic numbers
Show answer

2, 8, 20, 28, 50, 82, 126 — proton or neutron counts that fill nuclear shells and give extra stability.

Nuclear binding energy
Show answer

The energy released forming a nucleus from its nucleons; the mass defect times c2 c^2 . Iron-56 has the highest binding energy per nucleon.

Alpha, beta, gamma decay
Show answer

Alpha emits a X24X2224He \ce{^4_2He} nucleus; beta emits an electron/positron (plus a neutrino); gamma emits a high-energy photon.

Radioactive decay law
Show answer

N(t)=N0e−λt N(t) = N_0 e^{-\lambda t} ; the half-life is t1/2=ln⁡2λ t_{1/2} = \dfrac{\ln 2}{\lambda} .

Color confinement
Show answer

Quarks carry color charge and can never be isolated — only color-neutral hadrons (mesons, baryons) are observed.

Quark model
Show answer

Baryons are three quarks (e.g. proton = uud), mesons are a quark-antiquark pair; the six flavors are u, d, c, s, t, b.

The four fundamental forces
Show answer

Strong, electromagnetic, weak, and gravity — mediated by gluons, photons, W/Z bosons, and (hypothetically) gravitons.

Superconductivity
Show answer

Zero electrical resistance below a critical temperature; expels magnetic fields (Meissner effect).

Superfluidity
Show answer

Flow with zero viscosity, seen in liquid helium-4 below 2.17 K — particles flow without losing kinetic energy.

Chandrasekhar limit
Show answer

The maximum white-dwarf mass (≈ 1.4 solar masses) supported by electron degeneracy pressure; above it the core collapses.

References

  1. 1.ETS. “GRE Subject Tests: Content and Structure.” ETS. ↑
  2. 2.ETS. “GRE Physics Test Practice Book.” ETS. ↑
  3. 3.NIST. “The NIST Reference on Constants, Units, and Uncertainty.” National Institute of Standards and Technology. ↑
Career Employer

Career Employer is the ultimate resource to help you get started working the job of your dreams. We cover topics from general career information, career searching, exam preparation with free study materials, career interviewing, and becoming successful in your career of choice.

Follow Us:

All Posts

Career Employer’s Editorial Process

Here at Career Employer, we focus a lot on providing factually accurate information that is always up to date. We strive to provide correct information using strict editorial processes, article editing, and fact-checking for all of the information found on our website. We only utilize trustworthy and relevant resources. To find out more, make sure to read our full editorial process page here.