IB Physics memorize

Size of an atom

10^-10 m

Size of an nucleus

10^-15 m

Size of the universe

10^26 m

The three laws of newton

1. An object at motion will stay at motion, an object at rest will stay at rest unless a external force is applied.

2. F=ma (acceleration is porportional to F but inversly porportional to m)

3. Action and Reaction

Heat

energy tranfored from one body to another as a difference in temperature

Way to transfer heat

1. Convection (heat transfered through fluids)

2. Radiation (heat transfered through electromagnetic waves)

3. Conduction (heat transfered throgh direct contact, molecules)

Ideal gas characteristics

1. Particles have no size/volume

2. Obey laws of mechanics (elastic collisions)

3. No intermolecular forces

Thermodynamic processes

1. Isothermal - no temperature change

2. Isobaric - constant pressure

3. Isovolumetric (Isochoric) - constant volume

4. Adiabatic - no heat exchange (P(V^5/3) = constant, and T(V^2/3) = constant)

First law of thermodynamics

Conservation of energy in terms of themodynamic processes (ΔU=Q-W this is when work is done by the gas and energy is given to the gas and ΔU=Q+W is when work is done on the gas and energy is lost from the gas)

Second Law of thermodynamics

1. Entropy always increases in the universe

2. No engine in the universe is 100% efficient

Frame of reference

A system for specifying the precise location of objects in space and time

Inertia fram of reference

A frame of reference that is not accelerated

Muon Decay

Real world example of relativic effects.

Invariant quantaties

Quantities that do not change between inertail frames

Simple harmonic motion

a=-(w^2)x

Longitudinal and transversal waves

Describes the motion of the particle compared to the movement of the wave (longitudinal it is parallel (compression and rarefaction) while transversal is perpendicular)

Law of reflection

The incident angle, wavelength, and frequency equals the reflected angle, wavelength, and frequency

Refraction (Snell's law)

The bending of a wave as it passes at an angle from one medium to another

Diffraction

The bending of a wave as it moves around an obstacle or passes through a narrow opening

Standing waves

The superposition of two traveling waves, the incoming wave and the reflected (f=(vn)/(2L) or f=(vn)/(4L))

Doppler effect

The change in frequency of a wave as its source moves in relation to an observer

Way to transfer electric charge

1. By friction (objects become oppositely charge)

2. By contact (objects become the same charge)

3. By induction (objects become oppositely charge)

Electric field strength and gravitational field strength

1. The electric force per unit charge in a certain region in space

2. The gravitational force per unit mass in a certain region in space (Remember it is negative)

Field strength is the negative derivative of potential

Electric potential and gravitational potential

1. Work per unit of charge

2. Work per unit of mass (Remember it is negative)

Electrostatic inside conductors

1. E = 0 inside any conductor

2. E is always perpendicular to the surface outside a conductor

Inside non-conducting solid sphere: E increases until the surface and drops as you move away from the sphere.

Spherical shell conductor: E inside the shell is zero and acts normal from the surface and farther away.

Newtons's universal law of gravitation

The gravitational force of attraction between two masses is directly proportional to the masses and inversely proportional to the distance separation squared (F = G(m1m2)/r^2)

Kepler's law

1. All planets follow an elliptical trajectory

2. Planets sweep out equal areas in equal time intervals

3. T^2/r^ = constant

Resistance of a cable

R = pL/A

Diagram to find internal resistance

Battery connected to a varaible resistor which is parallel to a voltmeter, and then in series to an ammeter.

Ideal voltmeter

Infinite resistance

Ideal ammeter

Zero resistance

Magnetic field

a region in space in which a magnetic force i exerted (B with units tesla)

Magnetic field strength

Magnitude of the magnetic field at a point in space

Faraday's law

Induced emf is the change of magnetic flux over a change of time.

Lenz's law

The direction of the induced e.m.f. or current is always such as to oppose the change producing it (Nature law aka)

Nucleons

Protons and Neutrons

Isotopes of hydrogen

1. Hydrogen (1 proton and 1 neutron)

2. Deuterium (1 proton and 2 neutrons)

3. Tritium (1 proton and 3 neutrons)

Strong nuclear forces

The force that keeps protons together in the nucleous

Mass defect

Δm = (mp + mn)-m(nucleus)

Binding energy

Energy needed to split the nucleus into its individual components.

Radioactivity

Unstable nucleus is one that randomly and spontaneously emits particle that carry energy away from the nucleus.

Types:

1. Alpha decay = Helium ((4 2)He)

2. Beta-minus decay = ((0 -1)e) + ((0 0)anti-neutrino)

3. Beta-plus decay = ((0 +1)e(positrion)) + ((0 0)neutrino)

4. Gamma decay = unexcited nucleus + ((0 0)gamma)

Geiger-marsden experiment

Gold foil experiment

Bohrs model proof

Emission and absorption spectrum

Background radiation

The detector that measures the activity from a radioactive sampel also measures the activity from natural sources.

de Broglie wavelength

Wave-particle duality.

Compton effect

Waves collide with electrons (collision and energy tranfered)

Photo electric effect

Complete energy transfer of photons to electrons to complete the circuit. Classical vs modern

Davisson and Germer experiment

An experiment showing that electrons are scattered off crystals as a diffraction pattern due to the lattice structure, also known as "electron diffraction"

Nuclear power plant

1. Control rods (absorb neutrons to stop the chain reaction)

2. Moderator (slows down neutrons to continue the chain reaction)

3. Fuel rods (contain the uranium to have the chain reaction)

4. Heat exchanger (self-explanatory)

Luminosity vs brightness

1. Luminosity is power basically

2. Brightness is the power peer unit area

Black body

An ideal body which is both a perfect absorber and emitter of radiation. Classical vs modern

Important for P = σAT^4 used surface are

Parallax

Visual effect where the position an object relative to a background appears to change based on the viewers position.

Hydrostatic equilibrium

The balance of the inward gravitational force and the outward force of fusion within a star. This balance of forces is what keeps a main sequence star stable.

Evolution of Stars

Just remember 8 or more solar mass is high mass/massive star (iron)if less than 8 solar mass it is low and medium mass star (carbon or oxygen).

Neutrinium

Evidence of Proton-proton chain

H-R diagram

As you move to the left of the main sequence the mass increase.

Sun is 1 L and around 4900K.

The bigger the star the life expectancy decreases because it uses fule faster or more.

Albedo

The measure of the extent that an object can reflect radiation rather than absorb.

Temperature of Earth

Sπr^2(1-albedo)=eσ(4πr^2)T^4

Greenhouse gasses

1. Methane (Wetlands/Agriculture)