Exploring the Cosmos - Class Test 3 - Life and Death of Stars (Part 2)
1. The Crab Nebula is of interest because it
contains a pulsar.
contains a black hole.
is in the centre of the constellation Cancer.
surrounds the supernova SN1987A.
2. A globular cluster in our Galaxy is
a constellation such as Orion.
a group of very young stars.
an asterism like the Pleiades.
a group of very old stars.
3. Type I and II supernovae
can reoccur.
are both standard candles.
will occur in stars more massive than the Sun.
will occur in stars less massive than the Sun.
4. The main sequence is
the succession of stages in the life of a star.
a nuclear reaction in very hot stars.
a line on a graph of luminosity against temperature.
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5. An open cluster in our Galaxy is
most likely to be found in the galactic halo.
a constellation such as Orion.
a group of newly formed stars.
a group like the Pleiades.
6. White dwarfs
are very small in number.
are very hot.
are the remains of stars much less massive than the Sun.
are low magnitude stars.
7. Hydrogen burning in stars
produces water vapour in interstellar space.
is a nuclear reaction only occurring in the hottest stars.
is a reaction in which hydrogen fuses with oxygen.
can occur in the proton-proton chain reaction.
8. One element not expected to be produced in the core of stars is
gold.
silicon.
carbon.
helium.
9. Gas clouds contract to form stars because of
gravity.
nuclear forces.
electrical attraction.
internal pressure.
10. Stars in a single cluster differ widely in
chemical composition.
age.
mass.
distance.
11. Which of the following elements is not expected to be common in the core of a white dwarf?
Oxygen
Hydrogen
Carbon
Silicon
12. The CNO cycle is a nuclear reaction which
occurs in stars with cores hotter than the Sun.
occurs in carbon white dwarfs.
causes the helium flash.
produces 'metals'.
13. The final state of a star depends mainly on its
magnitude.
degeneracy.
mass.
chemical composition.
14. T Tauri stars are
standard candles.
frequently strong infrared sources.
remnant cores of dead stars.
optically visible in their cocoon.
15. Given that the radius of the Sun is about 700,000 km
light takes 2 to 3 seconds to travel from the core to the photosphere.
energy from fusion appears almost instantly at the photosphere.
energy from fusion takes about 1 million years to travel this distance.
it takes a few hours for light to travel from the core to the photosphere.
16. Protostars heat up mostly due to
radioactivity.
nuclear fission.
gravitational contraction.
nuclear fusion.
17. If 4 hydrogen nuclei fuse to form a helium nucleus
the mass-energy increases by about 1%.
the mass drops by about 1%.
the mass is conserved.
energy is absorbed.
18. The Chandrasekhar limit is
around ten times the solar mass.
the radius of a black hole.
the maximum radius of a red giant.
the maximum mass of a white dwarf.
19. Type I and II supernovae
can reoccur.
will occur in stars more massive than the Sun.
are both standard candles.
will occur in stars less massive than the Sun.
20. Type Ia supernovae are
are thought to be exploding white dwarfs.
very bright, newly-formed stars.
caused by stars collapsing upon themselves.
have strong H lines.
21. When the Sun becomes a Red Giant
its surface will become hotter than it is now.
it will eventually become a supernova.
it will produce iron and heavier elements in its core.
hydrogen fusion in its core will have ceased.
22. Which of the following elements is not expected to be common in the core of a white dwarf?
Carbon
Hydrogen
Oxygen
Silicon
23. The triple-alpha reaction is
an intermediate stage in the Carbon-Oxygen-Nitrogen cycle.
responsible for the formation of globular clusters.
a nuclear reaction in which helium fuses to form carbon.
an intermediate stage in the proton-proton chain reaction.
24. The supernova SN1987A
was at the same position as a previously catalogued star.
was seen in the nearby Andromeda galaxy.
emitted gravitational radiation which was detected on Earth.
is the most distant supernova seen until now.
25. One element not expected to be produced in the core of stars is
helium.
gold.
carbon.
silicon.
26. The supernova SN1987A
was seen in the nearby Andromeda galaxy.
is the most distant supernova seen until now.
emitted gravitational radiation which was detected on Earth.
was at the same position as a previously catalogued star.
27. The Chandrasekhar limit is
around ten times the solar mass.
the maximum mass of a white dwarf.
the maximum radius of a red giant.
the radius of a black hole.
28. Black holes
are caused absorption of light in cold, dense nebulae.
are the final stages of stars like the Sun.
cannot be directly observed.
are detected as dark clouds at the centre of galaxies.
29. The Schwarzschild radius gives
the size of a black hole.
the size of a neutron star.
the maximum size of a white dwarf.
the radius of the observable Universe.
30. Type I and II supernovae
will occur in stars less massive than the Sun.
will occur in stars more massive than the Sun.
can reoccur.
are both standard candles.
31. The Pauli Exclusion Principle explains
supernovae.
why neutron stars collapse.
the solar neutrino problem.
why white dwarfs are stable.
32. The final state of a star depends mainly on its
degeneracy.
magnitude.
mass.
chemical composition.
33. One element not expected to be produced in the core of stars is
silicon.
helium.
carbon.
gold.
34. The position of white dwarfs on a HR diagram is
at random points on the diagram.
to the lower left of the main sequence.
on the upper part of the main sequence.
to the right of the main sequence.
35. When the Sun becomes a Red Giant
it will eventually become a supernova.
it will produce iron and heavier elements in its core.
hydrogen fusion in its core will have ceased.
its surface will become hotter than it is now.
36. The CNO cycle is a nuclear reaction which
produces 'metals'.
occurs in carbon white dwarfs.
occurs in stars with cores hotter than the Sun.
causes the helium flash.
37. Black holes
exert a strong gravitational pull.
can only exist at the centres of galaxies.
are massive neutron stars.
are also called accretion disks.
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