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A.5 – General relativity (HL only)
Description
Nature of science:
Creative and critical thinking: Einstein’s great achievement, the general theory of relativity, is based on intuition, creative thinking and imagination, namely to connect the geometry of spacetime (through its curvature) to the mass and energy content of spacetime. For years it was thought that nothing could escape a black hole and this is true but only for classical black holes. When quantum theory is taken into account a black hole radiates like a black body. This unexpected result revealed other equally unexpected connections between black holes and thermodynamics. (1.4)
Understandings:
- The equivalence principle
- The bending of light
- Gravitational redshift and the Pound–Rebka–Snider experiment
- Schwarzschild black holes
- Event horizons
- Time dilation near a black hole
- Applications of general relativity to the universe as a whole
Applications and skills:
- Using the equivalence principle to deduce and explain light bending near massive objects
- Using the equivalence principle to deduce and explain gravitational time dilation
- Calculating gravitational frequency shifts
- Describing an experiment in which gravitational redshift is observed and measured
- Calculating the Schwarzschild radius of a black hole
- Applying the formula for gravitational time dilation near the event horizon of a black hole
Guidance:
- Students should recognize the equivalence principle in terms of accelerating reference frames and freely falling frames
Data booklet reference:
Theory of knowledge:
- Although Einstein self-described the cosmological constant as his “greatest blunder”, the 2011 Nobel Prize was won by scientists who had proved it to be valid through their studies on dark energy. What other examples are there of initially doubted claims being proven correct later in history?
Utilization:
- For the global positioning system to be so accurate, general relativity must be taken into account in calculating the details of the satellite’s orbit
- The development of the general theory of relativity has been used to explain the very large-scale behaviour of the universe as a whole with far-reaching implications about the future development and fate of the universe
Aims:
- Aim 2: the general theory of relativity is a great synthesis of ideas that are required to describe the large-scale structure of the universe
- Aim 9: it must be appreciated that the magnificent Newtonian structure had serious limitations when it came to the description of very detailed aspects of planetary motion
Directly related questions
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20N.3.HL.TZ0.7b(ii):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) if the tower and detector were accelerating towards the gamma rays in free space.
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20N.3.HL.TZ0.7b(ii):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) if the tower and detector were accelerating towards the gamma rays in free space.
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20N.3.HL.TZ0.b(ii):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) if the tower and detector were accelerating towards the gamma rays in free space.
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17N.3.HL.TZ0.8b:
Calculate the number of ticks detected in 10 ks by the distant observer.
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17N.3.HL.TZ0.8b:
Calculate the number of ticks detected in 10 ks by the distant observer.
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17N.3.HL.TZ0.b:
Calculate the number of ticks detected in 10 ks by the distant observer.
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18M.3.HL.TZ1.7c:
Observer A now sends a beam of light initially parallel to the surface of the planet.
Explain why the path of the light is curved.
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18M.3.HL.TZ1.7c:
Observer A now sends a beam of light initially parallel to the surface of the planet.
Explain why the path of the light is curved.
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18M.3.HL.TZ1.c:
Observer A now sends a beam of light initially parallel to the surface of the planet.
Explain why the path of the light is curved.
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18M.3.HL.TZ1.7a:
Calculate the shift in frequency observed by A in terms of Δf.
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18M.3.HL.TZ1.7a:
Calculate the shift in frequency observed by A in terms of Δf.
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18M.3.HL.TZ1.a:
Calculate the shift in frequency observed by A in terms of Δf.
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18M.3.HL.TZ2.7a.i:
Outline what is meant by the event horizon of a black hole.
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18M.3.HL.TZ2.7a.i:
Outline what is meant by the event horizon of a black hole.
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18M.3.HL.TZ2.a.i:
Outline what is meant by the event horizon of a black hole.
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18M.3.HL.TZ2.7b:
Star S-2 is in an elliptical orbit around a black hole. The distance of S-2 from the centre of the black hole varies between a few light-hours and several light-days. A periodic event on S-2 occurs every 5.0 s.
Discuss how the time for the periodic event as measured by an observer on the Earth changes with the orbital position of S-2.
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18M.3.HL.TZ2.7b:
Star S-2 is in an elliptical orbit around a black hole. The distance of S-2 from the centre of the black hole varies between a few light-hours and several light-days. A periodic event on S-2 occurs every 5.0 s.
Discuss how the time for the periodic event as measured by an observer on the Earth changes with the orbital position of S-2.
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18M.3.HL.TZ2.b:
Star S-2 is in an elliptical orbit around a black hole. The distance of S-2 from the centre of the black hole varies between a few light-hours and several light-days. A periodic event on S-2 occurs every 5.0 s.
Discuss how the time for the periodic event as measured by an observer on the Earth changes with the orbital position of S-2.
- 18N.3.HL.TZ0.7a.i: State what is meant by the event horizon of a black hole.
- 18N.3.HL.TZ0.7a.i: State what is meant by the event horizon of a black hole.
- 18N.3.HL.TZ0.a.i: State what is meant by the event horizon of a black hole.
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18N.3.HL.TZ0.7a.ii:
The mass of the black hole is 4.0 × 1036 kg. Calculate the Schwarzschild radius of the black hole.
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18N.3.HL.TZ0.7a.ii:
The mass of the black hole is 4.0 × 1036 kg. Calculate the Schwarzschild radius of the black hole.
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18N.3.HL.TZ0.a.ii:
The mass of the black hole is 4.0 × 1036 kg. Calculate the Schwarzschild radius of the black hole.
- 19M.3.HL.TZ1.7b.ii: State and explain the path of the light ray according to observer Y.
- 19M.3.HL.TZ1.7b.ii: State and explain the path of the light ray according to observer Y.
- 19M.3.HL.TZ1.b.ii: State and explain the path of the light ray according to observer Y.
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19N.3.HL.TZ0.6b:
The probe emits 20 short pulses of these radio waves every minute, according to a clock in the probe. Calculate the time between pulses as measured by the observer.
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19N.3.HL.TZ0.6b:
The probe emits 20 short pulses of these radio waves every minute, according to a clock in the probe. Calculate the time between pulses as measured by the observer.
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19N.3.HL.TZ0.b:
The probe emits 20 short pulses of these radio waves every minute, according to a clock in the probe. Calculate the time between pulses as measured by the observer.
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17N.3.HL.TZ0.8a:
Outline why the clock near the black hole runs slowly compared to a clock close to the distant observer.
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17N.3.HL.TZ0.8a:
Outline why the clock near the black hole runs slowly compared to a clock close to the distant observer.
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17N.3.HL.TZ0.a:
Outline why the clock near the black hole runs slowly compared to a clock close to the distant observer.
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18M.3.HL.TZ1.7b:
Calculate the gravitational field strength on the surface of planet X.
The following data is given:
Δf = 170 Hz.
The distance between observer A and B is 10 km.
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18M.3.HL.TZ1.7b:
Calculate the gravitational field strength on the surface of planet X.
The following data is given:
Δf = 170 Hz.
The distance between observer A and B is 10 km.
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18M.3.HL.TZ1.b:
Calculate the gravitational field strength on the surface of planet X.
The following data is given:
Δf = 170 Hz.
The distance between observer A and B is 10 km.
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18M.3.HL.TZ2.7a.ii:
Calculate the distance of the event horizon of the black hole from its centre.
Mass of Sun = 2 × 1030 kg
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18M.3.HL.TZ2.7a.ii:
Calculate the distance of the event horizon of the black hole from its centre.
Mass of Sun = 2 × 1030 kg
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18M.3.HL.TZ2.a.ii:
Calculate the distance of the event horizon of the black hole from its centre.
Mass of Sun = 2 × 1030 kg
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18N.3.HL.TZ0.7b:
The probe is stationary above the event horizon of the black hole in (a). The probe sends a radio pulse every 1.0 seconds (as measured by clocks on the probe). The spacecraft receives the pulses every 2.0 seconds (as measured by clocks on the spacecraft). Determine the distance of the probe from the centre of the black hole.
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18N.3.HL.TZ0.7b:
The probe is stationary above the event horizon of the black hole in (a). The probe sends a radio pulse every 1.0 seconds (as measured by clocks on the probe). The spacecraft receives the pulses every 2.0 seconds (as measured by clocks on the spacecraft). Determine the distance of the probe from the centre of the black hole.
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18N.3.HL.TZ0.b:
The probe is stationary above the event horizon of the black hole in (a). The probe sends a radio pulse every 1.0 seconds (as measured by clocks on the probe). The spacecraft receives the pulses every 2.0 seconds (as measured by clocks on the spacecraft). Determine the distance of the probe from the centre of the black hole.
- 19M.3.HL.TZ2.9a: Explain why a change in frequency is expected for the photon detected at the top of the rocket.
- 19M.3.HL.TZ2.9a: Explain why a change in frequency is expected for the photon detected at the top of the rocket.
- 19M.3.HL.TZ2.a: Explain why a change in frequency is expected for the photon detected at the top of the rocket.
- 19M.3.HL.TZ2.9b: Calculate the frequency change.
- 19M.3.HL.TZ2.9b: Calculate the frequency change.
- 19M.3.HL.TZ2.b: Calculate the frequency change.
- 19M.3.HL.TZ1.7a: State the equivalence principle.
- 19M.3.HL.TZ1.7a: State the equivalence principle.
- 19M.3.HL.TZ1.a: State the equivalence principle.
- 19M.3.HL.TZ1.7b.i: State and explain the path of the light ray according to observer X.
- 19M.3.HL.TZ1.7b.i: State and explain the path of the light ray according to observer X.
- 19M.3.HL.TZ1.b.i: State and explain the path of the light ray according to observer X.
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19N.3.HL.TZ0.6a:
Explain why the frequency of the radio waves detected by the observer is lower than .
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19N.3.HL.TZ0.6a:
Explain why the frequency of the radio waves detected by the observer is lower than .
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19N.3.HL.TZ0.a:
Explain why the frequency of the radio waves detected by the observer is lower than .
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20N.3.HL.TZ0.7a:
Calculate the fractional change in frequency of the gamma rays at the detector.
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20N.3.HL.TZ0.7a:
Calculate the fractional change in frequency of the gamma rays at the detector.
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20N.3.HL.TZ0.a:
Calculate the fractional change in frequency of the gamma rays at the detector.
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20N.3.HL.TZ0.7b(i):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) in the Earth’s gravitational field.
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20N.3.HL.TZ0.7b(i):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) in the Earth’s gravitational field.
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20N.3.HL.TZ0.b(i):
Explain the cause of the frequency shift for the gamma rays in your answer in (a) in the Earth’s gravitational field.