Transcript Chapter 16 Q&A - Personal.psu.edu

Question 1
The visible light we see
from our Sun comes
from which part?
1) core
2) corona
3) photosphere
4) chromosphere
5) convection zone
Question 1
The visible light we see
from our Sun comes
from which part?
1) core
2) corona
3) photosphere
4) chromosphere
5) convection zone
The photosphere is a
relatively narrow layer below
the chromosphere and
corona, with an average
temperature of about 6000 K.
Question 2
The density of the
Sun is most
similar to that of
1) a comet.
2) Jupiter.
3) the Earth.
4) interstellar gas.
5) an asteroid.
Question 2
The density of the
Sun is most
similar to that of
1) a comet.
2) Jupiter.
3) the Earth.
4) interstellar gas.
5) an asteroid.
The Sun is a ball of
charged gas, without a
solid surface.
Jupiter has a similar
composition, but not
enough mass to be a
star.
Question 3
The Sun is
stable as a
star because
1) gravity balances forces from pressure.
2) the rate of fusion equals the rate of fission.
3) radiation and convection balance.
4) mass is converted into energy.
5) fusion doesn’t depend on temperature.
Question 3
The Sun is
stable as a
star because
1) gravity balances forces from pressure.
2) the rate of fusion equals the rate of fission.
3) radiation and convection balance.
4) mass is converted into energy.
5) fusion doesn’t depend on temperature.
The principle of
Hydrostatic Equilibrium
explains how stars
maintain their stability.
Question 4
The proton–proton cycle
involves what kind of
fusion process?
1) carbon (C) into oxygen (O)
2) helium (He) into carbon (C)
3) hydrogen (H) into helium (He)
4) neon (Ne) into silicon (Si)
5) oxygen (O) into iron (Fe)
Question 4
The proton–proton cycle
involves what kind of
fusion process?
1) carbon (C) into oxygen (O)
2) helium (He) into carbon (C)
3) hydrogen (H) into helium (He)
4) neon (Ne) into silicon (Si)
5) oxygen (O) into iron (Fe)
In the P-P cycle, four
Hydrogen nuclei
(protons) fuse into one
Helium nucleus,
releasing gamma rays
and neutrinos.
Question 5
If a neutrino can escape
from the solar core
within minutes, then
how long does it take a
photon to escape?
1) minutes
2) hours
3) months
4) hundreds of years
5) about a million years
Question 5
If a neutrino can escape
from the solar core
within minutes, then
how long does it take a
photon to escape?
1) minutes
2) hours
3) months
4) hundreds of years
5) about a million years
Gamma ray photons are
absorbed and re-emitted
continuously in the layers
above the core.
They gradually shift in
spectrum to visible and
infrared light at the
photosphere.
Question 6
What is probably
responsible for the
increase in temperature
of the corona far from
the Sun’s surface?
1) a higher rate of fusion
2) the Sun’s magnetism
3) higher radiation pressures
4) absorption of X-rays
5) convection currents
Question 6
What is probably
responsible for the
increase in temperature
of the corona far from
the Sun’s surface?
1) the higher rate of fusion
2) the Sun’s magnetism
3) higher radiation pressures
4) absorption of X-rays
5) convection currents
Apparently the Sun’s
magnetic field acts like a
pump to increase the
speeds of particles in
the upper corona.
Question 7
The number of
sunspots and solar
activity in general
peaks
1) every 27 days, the apparent rotation
period of the Sun’s surface.
2) once a year.
3) every 5 ½ years.
4) every 11 years.
5) approximately every 100 years.
Question 7
The number of
sunspots and solar
activity in general
peaks
1) every 27 days, the apparent rotation
period of the Sun’s surface.
2) once a year.
3) every 5 ½ years.
4) every 11 years.
5) approximately every 100 years.
The sunspot cycle shows a consistent 11-year pattern of
activity dating back more than 300 years.
Question 8
The “Solar
Neutrino Problem”
refers to the fact
that astronomers
1) cannot explain how the Sun is stable.
2) detect only one-third the number of
neutrinos expected by theory.
3) cannot detect neutrinos easily.
4) are unable to explain how neutrinos
oscillate between other types.
5) cannot create controlled fusion
reactions on Earth.
Question 8
The “Solar
Neutrino Problem”
refers to the fact
that astronomers
1) cannot explain how the Sun is stable.
2) detect only one-third the number of
neutrinos expected by theory.
3) cannot detect neutrinos easily.
4) are unable to explain how neutrinos
oscillate between other types.
5) cannot create controlled fusion
reactions on Earth.
Further experiments have
shown that solar neutrinos
can change into other types
that were not initially
detected.