D.3 – Cosmology

Description

Nature of science:

Occam’s Razor: The Big Bang model was purely speculative until it was confirmed by the discovery of the cosmic microwave background radiation. The model, while correctly describing many aspects of the universe as we observe it today, still cannot explain what happened at time zero. (2.7)

Understandings:

The Big Bang model
Cosmic microwave background (CMB) radiation
Hubble’s law
The accelerating universe and redshift (z)
The cosmic scale factor (R)

Applications and skills:

Describing both space and time as originating with the Big Bang
Describing the characteristics of the CMB radiation
Explaining how the CMB radiation is evidence for a Hot Big Bang
Solving problems involving z, R and Hubble’s law
Estimating the age of the universe by assuming a constant expansion rate

Guidance:

CMB radiation will be considered to be isotropic with
For CMB radiation a simple explanation in terms of the universe cooling down or distances (and hence wavelengths) being stretched out is all that is required
A qualitative description of the role of type Ia supernovae as providing evidence for an accelerating universe is required

Data booklet reference:

International-mindedness:

Contributions from scientists from many nations made the analysis of the cosmic microwave background radiation possible

Utilization:

Doppler effect (see Physics sub-topic 9.5)

Aims:

Aim 1: scientific explanation of black holes requires a heightened level of creativity
Aim 9: our limit of understanding is guided by our ability to observe within our universe

Directly related questions

20N.3.SL.TZ0.16b:
Outline how Hubble’s law is related to $z$ .
20N.3.SL.TZ0.16b:
Outline how Hubble’s law is related to $z$ .
20N.3.SL.TZ0.b:
Outline how Hubble’s law is related to $z$ .
20N.3.HL.TZ0.21b:
Outline how Hubble’s law is related to $z$ .
20N.3.HL.TZ0.21b:
Outline how Hubble’s law is related to $z$ .
20N.3.HL.TZ0.b:
Outline how Hubble’s law is related to $z$ .
18M.3.SL.TZ1.12b:
Estimate, in Mpc, the distance between the galaxy and the Earth.
18M.3.SL.TZ1.12b:
Estimate, in Mpc, the distance between the galaxy and the Earth.
18M.3.SL.TZ1.b:
Estimate, in Mpc, the distance between the galaxy and the Earth.
18N.3.HL.TZ0.19b:
Use the graph to determine the age of the universe in s.
18N.3.HL.TZ0.19b:
Use the graph to determine the age of the universe in s.
18N.3.HL.TZ0.b:
Use the graph to determine the age of the universe in s.
18N.3.SL.TZ0.13b:
Using the graph, determine in s, the age of the universe.
18N.3.SL.TZ0.13b:
Using the graph, determine in s, the age of the universe.
18N.3.SL.TZ0.b:
Using the graph, determine in s, the age of the universe.
18N.3.HL.TZ0.19a:
Outline how Hubble measured the recessional velocities of galaxies.
18N.3.HL.TZ0.19a:
Outline how Hubble measured the recessional velocities of galaxies.
18N.3.HL.TZ0.a:
Outline how Hubble measured the recessional velocities of galaxies.
19M.3.SL.TZ2.14aii:
A line in the hydrogen spectrum when measured on Earth has a wavelength of 486 nm. Calculate, in nm, the wavelength of the same hydrogen line when observed in the galaxy’s emission spectrum.
19M.3.SL.TZ2.14aii:
A line in the hydrogen spectrum when measured on Earth has a wavelength of 486 nm. Calculate, in nm, the wavelength of the same hydrogen line when observed in the galaxy’s emission spectrum.
19M.3.SL.TZ2.aii:
A line in the hydrogen spectrum when measured on Earth has a wavelength of 486 nm. Calculate, in nm, the wavelength of the same hydrogen line when observed in the galaxy’s emission spectrum.
19M.3.SL.TZ2.14b: Outline how observations of spectra from distant galaxies provide evidence that the universe is...
19M.3.SL.TZ2.14b: Outline how observations of spectra from distant galaxies provide evidence that the universe is...
19M.3.SL.TZ2.b: Outline how observations of spectra from distant galaxies provide evidence that the universe is...
19M.3.HL.TZ1.19b: Suggest why type I a supernovae were used in the study that led to the conclusion that the...
19M.3.HL.TZ1.19b: Suggest why type I a supernovae were used in the study that led to the conclusion that the...
19M.3.HL.TZ1.b: Suggest why type I a supernovae were used in the study that led to the conclusion that the...
19M.3.SL.TZ2.14b: Outline how observations of spectra from distant galaxies provide evidence that the universe is...
19N.3.SL.TZ0.11b(i):
Estimate the age of the universe in seconds using the Hubble constant H₀ = 70 km s^–1Mpc^–1.
19N.3.SL.TZ0.11b(i):
Estimate the age of the universe in seconds using the Hubble constant H₀ = 70 km s^–1Mpc^–1.
19N.3.SL.TZ0.b(i):
Estimate the age of the universe in seconds using the Hubble constant H₀ = 70 km s^–1Mpc^–1.
19N.3.SL.TZ0.11a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.SL.TZ0.11a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.SL.TZ0.a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.SL.TZ0.11b(ii):
Outline why the estimate made in (b)(i) is unlikely to be the actual age of the universe.
19N.3.SL.TZ0.11b(ii):
Outline why the estimate made in (b)(i) is unlikely to be the actual age of the universe.
19N.3.SL.TZ0.b(ii):
Outline why the estimate made in (b)(i) is unlikely to be the actual age of the universe.
19N.3.HL.TZ0.16a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.HL.TZ0.16a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.HL.TZ0.a(i): Outline how the light spectra of distant galaxies are used to confirm hypotheses about the...
19N.3.HL.TZ0.16a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
19N.3.HL.TZ0.16a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
19N.3.HL.TZ0.a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
17N.3.SL.TZ0.13a: Outline one reason for the difference in wavelength.
17N.3.SL.TZ0.13a: Outline one reason for the difference in wavelength.
17N.3.SL.TZ0.a: Outline one reason for the difference in wavelength.
17N.3.SL.TZ0.13b:
Determine the velocity of the galaxy relative to Earth.
17N.3.SL.TZ0.13b:
Determine the velocity of the galaxy relative to Earth.
17N.3.SL.TZ0.b:
Determine the velocity of the galaxy relative to Earth.
18M.3.SL.TZ1.12a:
Explain how international collaboration has helped to refine this value.
18M.3.SL.TZ1.12a:
Explain how international collaboration has helped to refine this value.
18M.3.SL.TZ1.a:
Explain how international collaboration has helped to refine this value.
18M.3.SL.TZ2.12a:
Estimate, using the data, the age of the universe. Give your answer in seconds.
18M.3.SL.TZ2.12a:
Estimate, using the data, the age of the universe. Give your answer in seconds.
18M.3.SL.TZ2.a:
Estimate, using the data, the age of the universe. Give your answer in seconds.
18M.3.SL.TZ2.12b:
Identify the assumption that you made in your answer to (a).
18M.3.SL.TZ2.12b:
Identify the assumption that you made in your answer to (a).
18M.3.SL.TZ2.b:
Identify the assumption that you made in your answer to (a).
18M.3.SL.TZ2.12c:
On the graph, one galaxy is labelled A. Determine the size of the universe, relative to its present size, when light from the galaxy labelled A was emitted.
18M.3.SL.TZ2.12c:
On the graph, one galaxy is labelled A. Determine the size of the universe, relative to its present size, when light from the galaxy labelled A was emitted.
18M.3.SL.TZ2.c:
On the graph, one galaxy is labelled A. Determine the size of the universe, relative to its present size, when light from the galaxy labelled A was emitted.
18N.3.SL.TZ0.13a:
Outline how Hubble measured the recessional velocities of galaxies.
18N.3.SL.TZ0.13a:
Outline how Hubble measured the recessional velocities of galaxies.
18N.3.SL.TZ0.a:
Outline how Hubble measured the recessional velocities of galaxies.
19M.3.SL.TZ2.14ai: A galaxy is 1.6 × 108 ly from Earth. Show that its recessional speed as measured from Earth is...
19M.3.SL.TZ2.14ai: A galaxy is 1.6 × 108 ly from Earth. Show that its recessional speed as measured from Earth is...
19M.3.SL.TZ2.ai: A galaxy is 1.6 × 108 ly from Earth. Show that its recessional speed as measured from Earth is...
19N.3.SL.TZ0.11a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
19N.3.SL.TZ0.11a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
19N.3.SL.TZ0.a(ii):
Light from a hydrogen source in a laboratory on Earth contains a spectral line of wavelength 122 nm. Light from the same spectral line reaching Earth from a distant galaxy has a wavelength of 392 nm. Determine the ratio of the present size of the universe to the size of the universe when the light was emitted by the galaxy.
20N.3.SL.TZ0.16a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
20N.3.SL.TZ0.16a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
20N.3.SL.TZ0.a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
20N.3.HL.TZ0.21a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
20N.3.HL.TZ0.21a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
20N.3.HL.TZ0.a:
The light from a distant galaxy shows that $z = 0.11$ .

Calculate the ratio $\frac{size of the universe when the light was emitted}{size of the universe at present}$ .
21N.1.SL.TZ0.30: Which is correct for a black-body radiator? A. The power it emits from a unit surface area...
21N.1.SL.TZ0.30: Which is correct for a black-body radiator? A. The power it emits from a unit surface area...

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D.3 – Cosmology

Description

Directly related questions

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