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2024 AQA A-Level PHYSICS 7408/3B Paper 3 Section B Verified Question Paper and Marking S, Exams of Physics

2024 AQA A-Level PHYSICS 7408/3B Paper 3 Section B Verified Question Paper and Marking Scheme Attached June 2024 A PHYSICS Paper 3 Section B Astrophysics Monday 17 June 2024 Materials For this paper you must have: • a pencil and a ruler • a scientific calculator • a Data and Formulae Booklet • a protractor. Instructions • Use black ink or black ball-point pen. • Fill in the boxes at the top of this page. Morning Time allowed: The total time for both sections of this paper is 2 hours. You are advised to spend approximately 50 minutes on this section. For Examiner’s Use Question Mark 1 • Answer all questions. • You must answer the questions in the spaces provided. Do not write outside the box around each page or on blank pages. • If you need extra space for your answer(s), use the lined pages at the end of this book. Write the question number against your answer(s). • Do all rough work in this book. Cross through any work you do not want to be marked

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2024 AQA A-Level PHYSICS 7408/3B Paper 3 Section B
Verified Question Paper and Marking Scheme Attached
June 2024
A
PHYSICS
Paper 3
Section B Astrophysics
Monday 17 June 2024 Morning
Materials
For this paper you must have:
a pencil and a ruler
a scientific calculator
a Data and Formulae Booklet
a protractor.
Instructions
Use black ink or black ball-point pen.
Fill in the boxes at the top of this page.
Answer all questions.
Time allowed: The total time for both
sections of this paper is
2 hours. You are advised to
spend approximately
50 minutes on this section.
You must answer the questions in the spaces provided. Do not write outside the
box around each page or on blank pages.
If you need extra space for your answer(s), use the lined pages at the end of this book. Write
the question number against your answer(s).
Do all rough work in this book. Cross through any work you do not want to be marked.
Show all your working.
Information
The marks for questions are shown in brackets.
The maximum mark for this paper is 35.
You are expected to use a scientific calculator where appropriate.
A Data and Formulae Booklet is provided as a loose insert.
For Examiner’s Use
Question
Mark
1
2
3
4
TOTAL
pf3
pf4
pf5
pf8
pf9
pfa
pfd
pfe
pff
pf12
pf13
pf14
pf15
pf16
pf17
pf18
pf19
pf1a
pf1b
pf1c
pf1d
pf1e
pf1f
pf20
pf21
pf22
pf23
pf24
pf25
pf26

Partial preview of the text

Download 2024 AQA A-Level PHYSICS 7408/3B Paper 3 Section B Verified Question Paper and Marking S and more Exams Physics in PDF only on Docsity!

2024 AQA A-Level PHYSICS 7408 /3B Paper 3 Section B

Verified Question Paper and Marking Scheme Attached June 2024

A

PHYSICS

Paper 3

Section B Astrophysics Monday 17 June 2024 Morning

Materials

For this paper you must have:

  • a pencil and a ruler
  • a scientific calculator
  • a Data and Formulae Booklet
  • a protractor.

Instructions

  • Use black ink or black ball-point pen.
  • Fill in the boxes at the top of this page.
  • Answer all questions.

Time allowed: The total time for both

sections of this paper is 2 hours. You are advised to spend approximately 50 minutes on this section.

  • You must answer the questions in the spaces provided. Do not write outside the

box around each page or on blank pages.

  • If you need extra space for your answer(s), use the lined pages at the end of this book. Write

the question number against your answer(s).

  • Do all rough work in this book. Cross through any work you do not want to be marked.
  • Show all your working.

Information

  • The marks for questions are shown in brackets.
  • The maximum mark for this paper is 35.
  • You are expected to use a scientific calculator where appropriate.
  • A Data and Formulae Booklet is provided as a loose insert.

For Examiner’s Use Question Mark 1 2 3 4 TOTAL

Do not write outside the Section B

Answer all questions in this section.

box

(^0 1) A student uses a refracting telescope in normal adjustment to make observations of Jupiter.

The telescope has an angular magnification of 75

. 1 The eyepiece has a focal length of 22 mm.

Determine the distance between the eyepiece and the objective lens.

[2 marks]

distance = m

0 1. 2 When viewed through the telescope, the image of Jupiter subtends an angle of 1.7 × 10−^2

rad.

Calculate, in km, the distance between the Earth and Jupiter. mean radius

of Jupiter = 7.0 × 10^4 km

[2 marks]

distance = km

Do not write outside the Turn over ► box

Do not write outside the (^0 2) The apparent change in position of a nearby star relative to distant stars is due to an box

effect known as parallax.

Figure 2 shows how parallax arises. As the Earth moves from point P to point Q , an

observer on the Earth sees the position of a nearby star S change in relation to distant

stars.

Figure 2

Angle A is the parallax angle. This angle can be used to determine the distance to a

nearby star, provided that the relative motion between the star and the Sun is

negligible between observations.

. 1 The distance from the Sun to S is 79 ly.

The Earth takes 6 months to move from point P to point Q.

Calculate, in degrees, angle A.

[2 marks]

A = °

Do not write outside the 0 3. (^1) Figure 3 shows the variation of intensity with wavelength for a star.^ box

Figure 3

Show that Figure 3 is consistent with a black-body temperature of about 6.0 × 10

3

K.

[2 marks]

. 2 The radius of the star is 9.6 × 10

6

m.

Calculate the power output of the star.

[2 marks]

power output = W

Do not write outside the 3

. Which row gives the type and spectral class of the star?

Tick (✓) one box.

[1 mark]

box

. The light from the star passes through an interstellar dust cloud before reaching Earth.

The reduction in intensity when light passes through a dust cloud is assumed to be

inversely proportional to the wavelength of the light.

An astronomer on the Earth estimates the black-body temperature of the star.

Discuss the effect that the dust cloud has on this estimate.

[2 marks]

Turn over ►

Type of star Spectral class

white dwarf F

main sequence G

red giant K

main sequence F

red giant G

white dwarf K

Do not write outside the

Turn over ►

(^0 4) The Earth is in the galaxy known as the Milky Way. The Andromeda Galaxy is one of^ box

the closest galaxies to the Milky Way.

. 1 The Andromeda Galaxy approaches the Milky Way at a speed of 110 km s

− 1 .

The distance between the galaxies is 770 kpc.

Discuss whether these data can be used to estimate an age for the Universe.

[2 marks]

0 4. 2 There is a supermassive black hole at the centre of the Andromeda Galaxy. The

mass of this black hole is 1.60 × 10

8 solar masses.

Calculate the radius of the event horizon of this black hole.

State an appropriate unit for your answer.

[3 marks]

radius =

unit =

Question 4 continues on the next page

Do not write outside the box

Do not write outside the (^0 4). 3 Scientists predict that a quasar will be produced as the Milky Way and the Andromeda box

Galaxy merge.

Explain what is meant by a quasar.

Go on to suggest why a quasar may be produced as galaxies merge.

In your answer you should:

  • describe the typical properties of a quasar
  • explain how observations of quasars provide evidence for these properties
  • suggest the process of quasar formation that is likely when two galaxies merge. [6 marks]

There are no questions printed on this page

DO NOT WRITE ON THIS PAGE

ANSWER IN THE SPACES PROVIDED

Do not write outside the box

Do not write outside the box Question

number

Additional page, if required. Write the question numbers in the left-hand margin.

Do not write outside the box Question

number

Additional page, if required. Write the question numbers in the left-hand margin.

Do not write outside the There are no questions printed on this page

DO NOT WRITE ON THIS PAGE

ANSWER IN THE SPACES PROVIDED

box

.

2 Version 1.

Particle Physics Waves

Properties of quarks

antiquarks have opposite signs

Type Charge

Baryon

number

Strangeness

u +^

2

e

3

1

3

d −^

1

e

3

1

3

s

1

e

3

1

3

Properties of Leptons

Lepton number

Particles: e

e ;^ 

Antiparticles: e+, e, 

Photons and energy levels

Mechanics

moments (^) moment = 𝐹𝑑

velocity and acceleration

equations of

motion

𝑣^2 = 𝑢^2 + 2 𝑎𝑠

𝑎𝑡^2

force 𝐹 = 𝑚𝑎

force

impulse 𝐹 Δ𝑡 = Δ(𝑚𝑣)

work, energy and power

𝑊 = 𝐹 𝑠 cos 𝜃

1 𝐸k = 𝑚 𝑣^2 2

Δ𝐸p = 𝑚𝑔Δℎ

∆𝑊 , 𝑃 = 𝐹 ∆𝑡

Materials

photon energy

photoelectricity ℎ𝑓 = ϕ + 𝐸k (max)

energy levels (^) ℎ𝑓 = 𝐸 1 – 𝐸 2

de Broglie wavelength

Class Name Symbol (^) Rest energy/MeV

photon photon 𝛾 0

lepton neutrino v e 0

v  0

electron e

muon 

mesons (^)  meson 

0

K meson K

K

0

baryons proton (^) p 938.

neutron (^) n 939.

wave speed 𝑐 = 𝑓𝜆 period

first harmonic

fringe spacing

diffraction grating

𝑑 sin 𝜃 = 𝑛

refractive index of a substance s , 𝑛 =

𝑐

𝑐s

for two different substances of refractive indices n 1 and n 2 ,

law of refraction 𝑛 1 sin 𝜃 1 = 𝑛 2 sin 𝜃 2

critical angle sin 𝜃 =

𝑛 2

for 𝑛 > 𝑛

c (^) 𝑛 1

1 2

density 𝜌 =

𝑚

𝑉

Hooke’s law 𝐹 = 𝑘 Δ𝐿

Young modulus =

𝑡𝑒𝑛𝑠𝑖𝑙𝑒 𝑠𝑡𝑟𝑒𝑠𝑠 𝑡𝑒𝑛𝑠𝑖𝑙𝑒 𝑠𝑡𝑟𝑎𝑖𝑛

𝐹 tensile stress = 𝐴 ∆𝐿 tensile strain = 𝐿

energy stored 𝐸 =

1

2

Version 1.7 3

AQA A-LEVEL PHYSICS DATA AND FORMULAE

Electricity

current and pd

resistivity

resistors in series (^) 𝑅T = 𝑅 1 + 𝑅 2 + 𝑅 3 + …

resistors in parallel

1

1

1

1

  • ⋯ 𝑅T 𝑅 1 𝑅 2 𝑅 3

power

2

𝑃 = 𝑉𝐼 = 𝐼^2 𝑅 =

emf

Gravitational fields

force between two masses

𝑟^2

gravitational field strength

magnitude of gravitational

field strength in a radial field

𝑟^2

work done Δ𝑊 = 𝑚Δ𝑉

gravitational potential

Electric fields and capacitors

Circular motion

force between two 1 𝑄 1 𝑄 2

point charges

4 𝜋𝜀 0 𝑟^2

force on a charge 𝐹 = 𝐸𝑄

field strength for a 𝑉

uniform field

work done

𝑟

Simple harmonic motion

field strength for a radial field

𝑟^2

electric potential (^) 𝑉 =

field strength (^) 𝐸 =

capacitance (^) 𝐶 =

capacitor energy

0 r 𝑑

1 1 1 𝑄^2

stored

𝐶𝑉^2 =

Thermal physics

capacitor charging 𝑄 = 𝑄 0 (1 − e

  • 𝑡 - 𝑡 𝑅𝐶 (^) )

decay of charge (^) 𝑄 = 𝑄 0 e 𝑅𝐶

energy to change temperature

time constant 𝑅𝐶

energy to change

state

gas law (^) 𝑝𝑉 = 𝑛𝑅𝑇

kinetic theory model

𝑝𝑉 = 𝑁𝑚 (𝑐rms)^2 3

kinetic energy of gas molecule

𝑚 (𝑐rms)^2 = 𝑘𝑇 = 2 2 2 𝑁A

magnitude of angular speed

centripetal acceleration

𝑣^2

𝑎 = = 𝜔^2 𝑟

centripetal force

𝑚𝑣^2

𝐹 = = 𝑚𝜔^2

acceleration 𝑎 = − 𝜔^2 𝑥

displacement 𝑥 = 𝐴 cos (𝜔𝑡)

speed 𝑣 = ± 𝜔 �(𝐴^2 − 𝑥^2 )

maximum speed (^) 𝑣max = 𝜔𝐴

maximum acceleration 𝑎max = 𝜔^2 𝐴

for a mass-spring system

for a simple pendulum