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AS level Physics > Module 5 > Flashcards

Module 5 Flashcards

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1
Q

Absolute Temperature

A

A temperature value relative to absolute zero.

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2
Q

Absolute Zero

A

The lowest possible temperature of a system, where no heat
remains and the particles in the system have no kinetic energy

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3
Q

Avogadro Constant

A

The number of particles that make up one mole of any gas.

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4
Q

Boltzmann Constant

A

A constant relating the average kinetic energy of the
particles in a gas, to the gas’ temperature.

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5
Q

Boyle’s Law

A

The pressure of an ideal gas is inversely proportional to its volume
when held at constant temperature.

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6
Q

Brownian Motion

A

The random motion of particles.

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7
Q

Change of Phase

A

The transitions between solids, liquids and gases. During a
change of phase, there is a change of internal energy but not temperature

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8
Q

Equation of State of an Ideal Gas

A

An equation linking pressure, volume, number
of moles, temperature and the ideal gas constant.

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9
Q

Gas

A

A phase of matter in which the particles are high energy and free to move.
Gases will fill the space they are placed in.

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10
Q

Internal Energy

A

The sum of the randomly distributed kinetic and potential
energies of the particles in a given system.

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11
Q

Kelvin

A

The unit of absolute temperature.

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12
Q

Liquid

A

A phase of matter in which the particles can slide over each other, but still
have forces of attraction between each other.

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13
Q

Solid

A

A phase of matter in which the particles can only vibrate about fixed
positions, due to strong intermolecular forces.

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14
Q

Specific Heat Capacity

A

The amount of energy required to increase the
temperature of 1kg of a substance by 1 Kelvin

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15
Q

Specific Latent Heat

A

The amount of energy required to change the state of 1kg
of a substance without a change of temperature.

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16
Q

Thermal Equilibrium

A

A stable state in which there is no thermal heat transfer
between two regions.

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17
Q

Angular Velocity

A

An object’s rate of change of angular position

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18
Q

Centripetal Acceleration

A

The acceleration of an object moving in circular motion.
Any object in circular motion must have an acceleration since the direction of the
object, and therefore the velocity of the object, is constantly changing

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19
Q

Centripetal Force

A

The resultant force responsible for an object moving in circular
motion. Centripetal forces always act towards the center of the object’s rotation.

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20
Q

Frequency

A

The inverse of time period. The number of rotations per unit time

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21
Q

Period

A

The time taken for one whole rotation

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22
Q

Radian

A

A unit of angle, where 2π equal to one complete angular rotation

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23
Q

Angular Frequency

A

A measure of an object’s angular displacement per unit time

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24
Q

Critical Damping

A

The form of damping that reduces the displacement of an
oscillating object to its equilibrium position in the quickest time possible and
without further oscillation

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25
Q

Damping

A

The dissipation of energy from an oscillating system. The consequence
is that the amplitude of oscillation will decrease. Damping occurs when a force
opposes the system’s motion.

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26
Q

Forced Oscillations

A

Repeated up and down oscillations, at the frequency of a
driver. The amplitude of oscillation is small at high frequencies and large at low frequencies.

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27
Q

Free Oscillations

A

Oscillations that are not caused by a driver. An object will
naturally oscillate at its natural frequency.

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28
Q

Isochronous Oscillator

A

An oscillator whose frequency is independent to amplitude

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29
Q

Natural Frequency

A

The frequency that a system naturally oscillates at when
there is no driving force

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30
Q

Overdamping

A

A type of damping where the system is damped more than
required to stop the oscillations. It takes longer for the system to return to
equilibrium than for critical damping.

31
Q

Resonance

A

Resonance occurs when the frequency of oscillations is equal to the
natural frequency of the oscillating system. The rate of energy transfer is at a
maximum during resonance

32
Q

Simple Harmonic Motion

A

Motion where the acceleration of an object is directly
proportional, and in the opposite direction, to its displacement

33
Q

Underdamping

A

A type of damping where energy is gradually removed from the
system and the amplitude of oscillations slowly decreases.

34
Q

Escape Velocity

A

The minimum velocity required by an object to be able to
escape a gravitational field of a mass when projected vertically from its surface.

35
Q

Field Lines

A

A line representing the path that a mass would take when placed
within the field.

36
Q

Geostationary Satellite

A

A satellite that orbits above the equator with a 24 hour
period, so it will always remain above the same position on the Earth. They orbit
approximately 36,000km above the surface of the Earth

37
Q

Gravitational Field Strength

A

The force per unit mass exerted on a small test
mass placed within the field.

38
Q

Gravitational Field

A

A region surrounding a mass in which any other object with
mass will experience an attractive force.

39
Q

Gravitational Potential Energy

A

The component of an object’s energy due to its
position in a gravitational field.

40
Q

Gravitational Potential

A

The work done per unit mass required to move a small
test mass from infinity to that point.

41
Q

Kepler’s First Law

A

All planets travel in elliptical orbits, centered around the sun.

42
Q

Kepler’s Second Law

A

All planets sweep out the same area in a given period of
time.

43
Q

Kepler’s Third Law

A

The square of a planet’s period is directly proportional to the
cube of its mean distance to the sun.

44
Q

Newton’s Law of Gravitation

A

The force between two masses is proportional to
the product of the masses involved and inversely proportional to the square of the
separation of the masses.

45
Q

Absorption Line Spectrum

A

A spectrum consisting of dark lines at specific
frequencies that have been absorbed by the gases present. Elements can only
absorb certain energies, and therefore frequencies, of photons

46
Q

Astronomical Unit

A

The mean distance of the earth to the sun.

47
Q

Big Bang Theory

A

The theory that the universe originated as a small, dense and
hot region that expanded and cooled forming the structures in the universe we see
today

48
Q

Black Hole

A

A law stating that the power output (luminosity) of a star is directly
proportional to its surface area and its absolute temperature to the 4th power.

49
Q

Chandrasekhar Limit

A

The maximum mass that a white dwarf star can have
whilst remaining stable.

50
Q

Comets

A

Concentrated clusters of ice and dust that travel through space. When
near the sun, they begin to melt and so leave a trail as they move.

51
Q

Continuous Spectrum

A

A spectrum that covers a full range of frequencies without
any gaps. The electromagnetic spectrum is an example of a continuous spectrum.

52
Q

Cosmological Principle

A

A principle stating that the universe is isotropic (same in
all directions to all observers) and homogenous (matter is distributed evenly).

53
Q

Dark Energy

A

An energy that is responsible for the acceleration in the expansion
of the universe which cannot be explained by any observable energy.

54
Q

Doppler Effect

A

The apparent change in the wavelength of a wave as the source
moves relative to an observer. For a source moving away the wavelength
increases, for a source moving towards the observer the wavelength decreases.

55
Q

Electron Degeneracy Pressure

A

The outwards force, resisting the inwards force
of gravity, produced as a result of multiple electrons not being able to exist in
identical states in an energy level.

56
Q

Emission Line Spectrum

A

A series of bright lines at specific frequencies that
have been emitted by the gases present. Elements can only release photons of
certain energies, and therefore frequencies.

57
Q

Galaxies

A

Collections of billions of stars, planets, gases and dust, held together by
gravitational attraction

58
Q

Hertzsprung-Russell Diagram

A

A visual representation of the lifecycle of a star. It
is a plot of luminosity against temperature

59
Q

Hubble’s Law

A

The speed of a galaxy moving away from ours is proportional to its
distance away from us. The constant of proportionality is Hubble’s constant

60
Q

Light-Year

A

The distance travelled through space by a photon in a year

61
Q

Nebula

A

A cloud of dust and gas in space

62
Q

Neutron Star

A

An incredibly dense star that is formed when the core of a large
star collapses. Protons and electrons are forced together under gravity to form
neutrons.

63
Q

Parsec

A

The distance at which the angle of parallax is 1 arcsecond

64
Q

Planet

A

A body that orbits around a star, in our case, the Sun.

65
Q

Planetary Satellites

A

Bodies that orbit a planet. The gravitational force of the
planet’s mass provides the centripetal force of rotation

66
Q

Red-Giant

A

A stage in the life cycle of a star less than 3 solar masses, in which
the hydrogen has run out and the temperature of the star increases. Helium nuclei
fuse to form heavier elements.

67
Q

Solar Systems

A

A collection of planets that orbit a common star

68
Q

Stefan’s Law

A

A law stating that the power output (luminosity) of a star is directly
proportional to its surface area and its absolute temperature to the 4th power.

68
Q

Stellar Parallax

A

The change in position of an object depending on the viewing
angle. It can be used to estimate the distance of a star, based on how much it
moves relative to the background of stars in the time it takes for the earth to move
half an orbit.

69
Q

Supernova

A

When a star greater than 1.4 solar masses dies, the core collapses
rapidly inward and becomes rigid. The outer layers then fall inward and rebound
off of the core in a shockwave, causing heavy elements to be fused and
distributed into space in an explosion

70
Q

Universe

A

The name given to all space and matter

71
Q

White Dwarf

A

A dense star, similar mass to the sun, similar size to the earth. A
final stage of a low mass star’s life with low luminosity

72
Q

Wien’s Displacement Law

A

A law stating that the peak wavelength of emitted
radiation is inversely proportional to its absolute temperature.

AS level Physics (14 decks)

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