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Further Physics Flashcards

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1
Q

Solar day

A

So today is the time taken between successive means = 24 hours

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2
Q

Lunar eclipse

A

This occurs when the Moon moves into the earth shadow. The eclipses are rare because the moon orbits the Earth at the angle about 5° to the Earth’s path around the sun

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3
Q

Solar eclipse

A

This occurs when the sun, moon and a line up so that the moon appears to block out the sun

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4
Q

Geocentric model

A

-ptolem = The earth at the centre of the solar system

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5
Q

Heliocentric model

A
  • capernicus = Sun at the centre of the solar system
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6
Q

How do you planets move

A

Retrograde motion

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7
Q

Retrograde motion

A

Distant planet take longer to complete their orbits them planet is closest to the sun. Consequently, the relative position change over time
E. G. Mars

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8
Q

What is constellation

A

A named group of stars that form a pattern in the sky as seen from Earth although the stars themselves usually have no connection with each other

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9
Q

Why can we see more stars in the night sky in summer than winter

A
  1. The earth has moved to the other side of its orbit around the sun.
  2. Nights are longer in winter and there are some very bright lights on show.
  3. In the summer months are night skies aim towards the centre of the Galaxy
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10
Q

What is the Milky Way

A

A band of light stretching from the north-east to the south west across the sky

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11
Q

Celestial sphere

A

An imaginary sphere with the earth at the centre, on which we imagine all astronomical objects are located

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12
Q

Celestial equator

A

The midline around the celestial sphere

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13
Q

Ecliptic

A

Path taken by the sun along the celestial to be in one year

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14
Q

Declination

A

The angle of the object above or below the celestial equator

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15
Q

Right ascension

A

Angle of the object along the celestial equator with the vernal equinox (point where the elliptic crosses the celestial equator) at zero

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16
Q

What is one arch minute

A

1/60 of a degree (1’)

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17
Q

What is 1 arch second

A

1/3600 year of a degree (1”)

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18
Q

Parallax

A

This is the effect whereby the position of an object appears to change when it is viewed from a moving source

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19
Q

What is the equation of the parallax angle

A

Parallax angle = Alpha + beta/2

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20
Q

What does the parallax angle show

A

The parallax angle allows us to find out the distance to stars which are close to earth

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21
Q

What is the relationship between the parallax angle and parsec

A

When the parallax angle is one of the second the distance is 1 parsec (pc)

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22
Q

The simple question for parsecs (pc)

A

Distance (in parsecs) = 1/ parallax angle (measured in arc seconds)

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23
Q

What factors affect the brightness of the star

A

. size
. temperature/age
. distance
. chemical composition

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24
Q

Intensity

A

Intensity of a source of radiation is the number of photons which fall on a surface every second

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25
Q

What are the properties of intensity

A
  1. The radiation spreads out as it moves away from the source
  2. this means that the intensity decreases with distance. In fact, it obeys the inverse square law, which means that the intensity decreases by value which is inversely proportional to its (distance)2
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26
Q

Sidereal day

A

It’s ideal day is the time taken for the F to rotate through 360° (measured against a very distant star) = 24 hours and 56 minutes

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27
Q

Heber Curtis hypothesis

A
  1. Heber Curtis argued for the island universe hypothesis.
  2. He said that the spiral nebulae were galaxies like our own
  3. he believed that our galaxy was only 30,000 ly across
  4. that our sun was near the centre of it
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27
Q

Harlow Shapley hypothesis

A

. Harlow Shapley thought our galaxy was much bigger, 300,000 ly across, and that it formed the whole universe
. he believed that the sun was not at the centre of the galaxy
. that the spiral nebulae were just clouds of gas, relatively small and nearby

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28
Q

What did Edwin Hubble look at

A
  1. Edwin Hubble looked at variable stars (Cepheid Variables) in the Adronema nebula 2. the cycle of brightness (period) was long, suggesting that the stars were very bright, but they appeared very dim from Earth suggesting that they were very long way away 3. this data suggests that nebulae are other galaxies and are a very long way away
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30
Q

Nebulae

A

Extended, cloud like, objects in space, for example galaxies or gas clouds

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31
Q

What did Henrietta Leavitt find

A

She found that there was a direct correlation between the brightness of a variable star and its PERIOD

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32
Q

What is the period of a star

A

The time it takes to complete a full cycle

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33
Q

How do we work out how far away a a star is

A

We can work out how far away a star or galaxy is by looking at nearby variable stars and applying the mathematical relationship between distance and velocity

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34
Q

What did Hubble’s graph show

A

• the correlation on the graph, that is :- all the galaxies are moveing away from each other and the further apart they are, the great the speed at which they are moving (recessional velocity)

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35
Q

What does redshift tell us

A

The stretching of light to longer wavelengths caused by the expansion, space, or by the recessional velocity of a source

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36
Q

What is the period of a cepheid variable

A

Is the time taken to go through a full cycle from bright to dim

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37
Q

Heber Curtis hypothesis

A
  1. Heber Curtis argued for the island universe hypothesis.
  2. He said that the spiral nebulae were galaxies like our own
  3. he believed that our galaxy was only 30,000 ly across and that our sun was near the centre of it
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38
Q

Harlow Shapley hypothesis

A
  1. Harlow Shapley thought our galaxy was much bigger, 300,000 ly across, and that it formed the whole universe
  2. he believed that the sun was not at the centre of the galaxy and that the spiral nebulae were just clouds of gas, relatively small and nearby
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39
Q

What did Henrietta Leavitt examine

A

Henrietta Leavit examined variable stars in the Greater and Lesser Magellanic Clouds- this meant that she knew they were all the same distance from us

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40
Q

Hubble and the Great Debate

A
  1. Edwin Hubble looked at variable stars (Cepheid Variables) in the Adronema nebula
  2. the cycle of brightness (period) was long, suggesting that the stars were very bright, but they appeared ver dim from Earth suggesting that they were very long way away
  3. these data suggest that nebulae are other galaxies and are a very long way away
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42
Q

Nebulae

A

Extended, cloud like, objects in space, for example galaxies or gas clouds

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43
Q

What did Henrietta Leavitt find

A

She found that there was a direct correlation between the brightness of a variable star and its PERIOD

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44
Q

What is the period of a star

A

The time it takes to complete a full cycle

45
Q

How do we work out how far away a a star is

A

We can work out how far away a star or galaxy is by looking at nearby variable stars and applying the mathematical relationship between distance and velocity

48
Q

What did Henrietta Leavitt examine

A

Henrietta Leavit examined variable stars in the Greater and Lesser Magellanic Clouds- this meant that she knew they were all the same distance from us

49
Q

What two pieces of information suggest the Big Bang

A
  1. red shift

2. cosmic background radiation

50
Q

How does redshift link with the spectrum

A

Objects moving away show light which appears to have shifted towards the red end of the spectrum

51
Q

What happens when light travels from one substance to another

A

Refraction- when light travels from one substance (medium) to another it may change speed.

  1. If the angle at which it approaches the second medium is 90° it will continue unchanged.
  2. At any other angle the light may change direction.
52
Q

Focal length

A

Th distance from the centre of the lens to the focal point

53
Q

Power of lens

A

Power of a lens tells us how good it is at refraction light

54
Q

Power triangle

A

Power= 1/ focal length (in metres)

55
Q

What is the unit and symbol for power

A

Symbol : P

Unit : Dioptres

56
Q

What do we have to remember when finding the power

A

ALWAYS CONVERT FOCAL LENGTH INTO DIOPTRES

57
Q

How does refraction occur been the light is parallel to the principal axis

A

A ray of light which is parallel to the principal axis is refracted through the focal point

58
Q

How does refraction occur when a ray of light passes through the the focal point

A

A ray of light passing through the focal point is refracted parallel to the principal axis

59
Q

How does refraction occur when a ray of light passes through the centre of curvature

A

A ray of light passing through the centre of curvature continues

60
Q

Objective lens

A

The (larger diameter) lens at the front of a refracting telescope

61
Q

Eyepiece

A

The (smaller diameter) lens through which the observer looks when using a telescope

62
Q

What does the objective and eyepiece lens have to be and why

A
  1. the objective lens has a larger diameter than the eyepiece because objective needs to have a large area to collect more light and make a bright and clear image, it forms an image of the object at its focal point
63
Q

Magnification equation

A

Magnification = focal length of objective lens/ focal length of eyepiece
Or fo/fe

64
Q

Chromatic aberration

A

The different colours that make up white light have different wavelengths. At any lens, each colour will be refracted by a different amount. This means that images may be surrounded by a coloured ‘fringe’ or blurring effect

65
Q

Name the problems with refracting telescopes

A
  1. Chromatic aberration

2. Over time glass flows, so lenses will become distorted

66
Q

Diffraction

A
  1. when waves pass through a gap (aperture) which is approximately one wavelength wide they spread out in a curved path
  2. this means that there maybe distortions effects at the edges of the lenses, mirrors etc.
    so a large lens will show fewer diffraction effects
67
Q

Ground state

A

The original energy level in an atom

68
Q

The absorption spectrum

A

An absorption spectrum has BLACK LINES on it where energy is absorbed from the radiation to raise some of the electrons to higher energy levels

69
Q

Emission spectrum

A

A emission spectrum has coloured lines on it where the energy that was absorbed is now released

70
Q

What does the spectral lines show us about the universe

A
  1. Spectral lines from other stars, and even from other galaxies are similar to that of our Sun
  2. This suggests their are stars like our sun in different galaxies, elements are the same throughout the universe (the Big Bang)
71
Q

What does the absence of certain light tell us e.g. Yellow light

A

There is no yellow light from this atom because only certain energy levels are allowed, so only certain colours are emitted

72
Q

Boyle’s law

A

If we increase the pressure on a gas it’s volume decreases. This occurs if we keep the temperature constant

73
Q

What does the boyles law mean in terms of graphs

A

This means that pressure is inversely proportional to volume
1. pV = constant

74
Q

Temperature

A

Is the measure of heat energy (movement of the constituent ((particles that make it up )))

75
Q

Absolute 0

A

Temperature at which particles have the minimum possible energy (-237 degrees centigrade)

76
Q

What is the pressure of a gas

A

The pressure of a gas is a measure of the number of times the particles collide with the walls of the container every second

77
Q

What happens to the pressure and temperature if we keep the volume of a gas constant

A

If we keep the volume of a gas constant we find that the pressure is directly proportional to the temperature
1. p/T = constant

78
Q

What happens when the volume when the temperature is increased at a constant pressure

A

When we increase the temperature at a constant pressure, we find that, as the temperature increases the volume decreased

79
Q

What do we always have to remember when using temperature in equations

A

USE KELVIN FOR TEMPERATURE NOT DEGREES CENTIGRADE

1. by adding 273 degrees centigrade

80
Q

The birth of a star

A
  1. A cloud of hydrogen forms in space
  2. Gravitational attraction causes the particles to move together
  3. The mass of particles increases its gravity as its gets bigger but also, as particles join the mass they increase its energy
  4. When the inward gravitational force equals the outward force which resolute fro the particles moving around more, we say the mad is in its equilibrium
  5. If some kind of change occurs, like a supernova (exploding star), then the mass may get even bigger
  6. Eventually it will gain sufficient energy to glow. This is called the protostar
  7. If the particles gain sufficient energy they release photons of energy as light, infra-red etc.
81
Q

Strong nuclear force

A

This is the force that holds protons and neutrons together in the nucleus

82
Q

Thermonuclear fusion

A
  1. This force only avid over s very small range (about 10 to the minus 15) but is strong enough to overcome electrostatic repulsion between the protons
  2. If particles have sufficient energy to approach close enough to the nucleus for the strong nuclear force to act on them they will fuse together and this releases energy
83
Q

How do we find the number of neutrons

A

Neutrons = larger - smaller

84
Q

How to determine which is which regarding printings, neutrons and electrons

A 
Smaller= atomic no. Of protons 
Larger = mass no. Of electrons and neutrons
85
Q

Plasma

A

A state of matter where the particles have so much energy that they spectate into protons, electrons and neutrons

86
Q

Name of hydrogen with a mass of 1,2 and 3

A
  1. Mass of 1 : hydrogen
  2. Mass of 2 : deuterium
  3. Mass of 3 : tritium
87
Q

How is deuterium formed

A

When two hydrogen nuclei collide at high energies they fuse to form deuterium and they lose mass so energy is released

88
Q

What is needed to make nuclei fuse

A

High temperatures are needed to make nuclei fuse because it requires high energy to overcome electrostatic repulsion:- the repulsive force between 2 positive nuclei

89
Q

What is Einstein’s equation

A

E = mc2

=> energy = mass x (speed of light) 2

90
Q

Mass defect

A

In a fusion reaction particles join together and lose mass. This loss in mass is called the mass defect

91
Q

Mass defect equation

A

Mass defect = 🔼m

So the energy released = 🔼mc2

92
Q

Properties of a massive star

A

• will had a greater gravity so theparticles will fuse with more energy which means that more energy is released

93
Q

Main sequence

A

The stage in a Stars life where the fusion of hydrogen into helium takes place in the core

94
Q

How is energy radiated into the Photosphere

A
  1. the photons of energy from the nuclear fusion taking place in the core of the star travel to the surface by radiation and convection
  2. this energy is then radiated from the surface of the sun (photosphere) into space
95
Q

How does a star keep it’s equilibrium

A

Gravity and gas pressure are the 2 forces which act on a star and keep it in equilibrium. Gravity is the inward force and has pressure is the outward force

96
Q

Hertsprung- Russell diagram

A
  1. Stars in the main sequence form a diagonal line
  2. For small/medium stars - run out of fuel (hydrogen) so the inward force (gravity) causes the star to collapse brief final episode of fusion and the star expands to form a red giant
  3. Eventually cool and contract to a white dwarf
  4. For large/huge stars - runs out of fuel and collapses, huge expansion (SUPERGIANT) collapses and explodes (NOVA OR SUPERNOVA) cools and contracts (NEUTRON STAR/ BLACK HOLE)
97
Q

Hubble’s law

A

Plot of the distances of stars from Earth and the speed which they are moving away from us

98
Q

What does Hubble’s law suggest

A

That the universe is expanding (evidence for the Big Bang)

99
Q

Equation from Hubble’s law graph

A 
Vr inversely proportional to distance 
OR 
Vr = constant x distance 
=> Vr = H0 x distance 
Where H0 = Hubble constant
100
Q

Equation for the age of the universe

A

Age of the universe = 1/H0

101
Q

Which colour represents the most and least energy in the Hertsprung- Russell diagram

A
  1. Blue indicates the most energy. 2. Red indicates the the least energy
102
Q

Which stars carry out the most hydrogen fusion

A

Stars in the MAIN SEQUENCE carry out hydrogen fusion

103
Q

Why aren’t BLACK HOLES on the Hertsprung-Russell diagram

A

BLACK HOLES are not on the Hertsprung Russell diagram because they have not luminosity

104
Q

Why is their a relationship between distances to far galaxies and their speeds of recession

A

The universe started with the Big Bang so is always expanding

105
Q

Why are scientists confident that the relationship between speed of recession and distance of far galaxies is correct

A

The data is the other theories and we are getting more data which proves the theory and the theory has not yet been disproven

106
Q

What is speed of recess also known as

A

Velocity

107
Q

Cepheid variable stars

A

A type of star with luminosity that varies in a regular way; the period of the variation depends on the size of the star

108
Q

How do we work out distance using variable stars

A

By comparing its real brightness with its apparent brightness

Physics 7 (2 decks)

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