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A-Levels > Physics Paper 1 > Flashcards

Physics Paper 1 Flashcards

1
Q

SI units

A

kg, m, s, Amps, Kelvin, mol

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2
Q

couple

A

pair of equal forces, act parallel but in opposite directions

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3
Q

torque of couple

A

1 force x total distance between the forces

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4
Q

spring constants in parallel

A

add

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5
Q

spring constants in series

A

add reciprocals

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6
Q

ultimate tensile strength

A

maximum stress material can take before breaking

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7
Q

area under stress-strain graph

A

energy per unit volume

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8
Q

limit of proportionality (stress-strain graph)

A

graph no longer straight, starts to curve and stops obeying Hooke’s law, but would still return to original shape if stress removed

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9
Q

elastic limit (stress-strain graph)

A

starts to behave plastically, material will no longer return to original shape if stress removed

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10
Q

yield point (stress-strain graph)

A

material suddenly starts to stretch without any extra load, stress at which a large amount of plastic deformation takes place with constant/reduced load

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11
Q

brittle (stress-strain graph)

A

doesn’t curve

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12
Q

stiffness & strength (stress-strain graph)

A

higher line goes - stronger
steeper the gradient - stiffer

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13
Q

Boyle’s law

A

pV = constant (constant temperature)

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14
Q

Charles’ law

A

constant pressure, V directly proportional to T

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15
Q

pressure law

A

p/T constant at constant volume

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16
Q

Boltzmann constant k

A

R/avagadro

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17
Q

kinetic theory assumptions

A
  • large N, rapid and random movement
  • volume particles < volume
  • collisions perfectly elastic
  • duration collision < between
  • no forces between particles except collisions
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18
Q

elastic v inelastic collision

A

momentum conserved in both, k.e. only in elastic

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19
Q

damping

A

critical - shortest possible time
light - light innit
very heavy - one very long half-oscillation
heavy - just a few

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20
Q

damping and resonance

A

light - very sharp resonance peak (amplitude v freq. graph)
heavy - flatter

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21
Q

Newton’s first law

A

velocity of object will not change unless resultant force applied

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22
Q

Newton’s second law

A

force is rate of change of momentum/ma

23
Q

Newton’s third law

A

equal but opposite

24
Q

Kepler’s first law

A

each planet moves in an ellipse, with the Sun at one focus

25
Q

Kepler’s second law

A

lines joining Sun to planets will sweep out equal areas in equal times

26
Q

Kepler’s third law

A

T^2 =kr^3

27
Q

AU

A

mean distance between Sun and Earth

28
Q

parsec

A

distance if angle of parallax is 1 arcsecond (1/3600)

29
Q

comet

A

few hundred metres to tens of kilometres, irregular and made of ice, dust and rock, highly eccentric elliptical orbits

30
Q

radiation pressure, gas pressure

A

from photons emitted during fusion, from nuclei in the core pushing out

31
Q

cosmological principle

A

on large scale, universe is homogeneous, isotropic (same in every direction), and laws of physics universal

32
Q

universe timeline (numbers orders of magnitude in seconds)

A

-35: inflation
-6: fundamental particles gain mass
-4: grand unified force splits, matter-antimatter symmetry breaks
-3: first hadrons
0 - creation of matter stops
2 - helium nuclei and deuterium nuclei form
380k years - atoms (EM can now travel freely - CMBR)
30m years - first stars

33
Q

H-R diagram

A

bottom left - white dwarfs
top right - red giants and super red giants
main sequences diagonal line top left to bottom right
luminosity y axis, temperature x axis (inverted)

34
Q

normal mass stellar evolution

A

red giant -> white dwarf

35
Q

heavy stellar evolution

A

super red giant -> white dwarf core -> (1.4x> Sol) -> supernova -> neutron star (1.4-3x Sol) or black hole (3x> Sol)

36
Q

Chandrasekhar limit

A

1.4x solar mass - maximum mass at which electron degeneracy pressure can counteract gravitational force of star

37
Q

red giant

A
  • H in core runs out, fusion and outward pressure stops
  • core contracts, heats up, outer layers cool
  • shell hydrogen burning (enough energy from core collapse)
  • core continues to contract until core helium burning, expanding outer layers
  • shell helium burning
38
Q

white dwarf

A
  • carbon-oxygen core (from red giant) isn’t hot enough for further fusion so continues to contract
  • if under 1.4x Sol (Chandrasekhar limit), helium shell becomes unstable as core contracts
  • star pulsates and ejects outer layers in nebula
39
Q

super red giant

A
  • onion-like structure of different fusions all the way up to iron
  • core then contracts and forms white dwarf core
  • if larger than Chandrasekhar limit, electron degeneracy pressure will not prevent further collapse
  • continues to contract, outer layers fall in and rebound creating a shockwave - a supernova
40
Q

graph of P against volume

A

1/x, at higher temps graph moves further from origin

41
Q

internal energy

A

sum of (random distribution of) kinetic and potential energies

42
Q

ideal gases energy

A

potential energy is negligible

43
Q

small amplitude oscillations (<10 degrees)

A

amplitude and time period independent

44
Q

energy levels sign

A

negative as represent energy electron must gain to leave atom

45
Q

amplitude-frequency graph

A
  • if heavier damping, will become flatter, possibly move a bit to left, but will NOT intersect original curve
  • will resonate at natural freq., and A will increase to it and decrease after
46
Q

centripetal force

A

perpendicular to motion, causing change in direction and circular motion

47
Q

semicircle prism experiment n

A

to find refractive index of material, shine laser at curved end and change angle until just on point of total internal reflection, when light ray comes outalong the straight side

48
Q

diffraction grating

A

screen at least 1m away, mean distance for maxima (reduce uncertainty in sin theta)
use screen distance as hypotenuse in calculations

49
Q

thinking distance

A

Distance travelled from the moment the driver sees a hazard until the brakes are applied
- proportional to speed for constant thinking/reaction time

50
Q

spring constant of halves when you cut a spring in half

A

2k

51
Q

how to make time a kettle boils shorter/more accurate to theoretical

A

lag the kettle (adding insulation), cover to prevent evaporation of water

52
Q

ball on slope determining g

A
  • Stop timer when ball reaches bottom of ramp.
  • Make distance as long as possible to reduce % uncertainty in timing.
  • Repeat measurement for t to get an average.
  • Mark the ramp at the set distance d to ensure release point is accurate.
  • Use a release mechanism to release ball.
  • Ensure the ball is not pushed when released.
53
Q

reason why normal and weight not 3rd law reaction pair

A

both forces act on same object

different kinds of force (grav. and electrostatic)

54
Q

gravitational potential definition

A

Work done per unit mass to move an object from infinity
(to that point)

A-Levels (4 decks)

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