Question 1

The fact that the currently observed $\Omega$mass + $\Omega$$\wedge$  is very close to 1 means that its value has always been very close to 1.

Accepted Answer

A) True 
 B)False

Question 2

If you found a globular cluster that had an age of 20 billion years, what cosmological observations would conflict with this observation?

Accepted Answer

The WMAP results on the CMB sa

Question 3

If there were no dark energy in the universe, the value of __________ would determine the evolution and fate of the universe.

Accepted Answer

A)  "H0" 
B)  "1/H0" 
C)  " $\Omega$luminous" 
D)  " $\Omega$mass" 
E)  " $\Omega$$\wedge$ " 
A)  "H0" 
B)  "1/H0" 
C)  " $\Omega$luminous" 
D)  " $\Omega$mass" 
E)  " $\Omega$$\wedge$ "

Question 4

To determine how the expansion rate of the universe has changed over time, astronomers directly measure the __________ for a sample of Type I supernovae in distant galaxies.

Accepted Answer

A)  redshift and luminosity 
B)  redshift and brightness 
C)  redshift and distance 
D)  distance and luminosity 
E)  distance and brightness 
A)  redshift and luminosity 
B)  redshift and brightness 
C)  redshift and distance 
D)  distance and luminosity 
E)  distance and brightness

Question 5

The concept of inflation helps solve both the problems of the flatness of the universe and smoothness of the cosmic background radiation.

Accepted Answer

A) True 
 B)False

Question 6

As the universe cooled shortly after the Big Bang, which was the first fundamental force to separate itself out from the others?

Accepted Answer

A)  electromagnetism 
B)  gravity 
C)  the nuclear force 
D)  the strong force 
E)  the weak force 
A)  electromagnetism 
B)  gravity 
C)  the nuclear force 
D)  the strong force 
E)  the weak force

Question 7

The flatness problem arises because only a universe with __________ can have that value forever.

Accepted Answer

A)  "$\Omega$mass + $\Omega$ $\wedge$  = 0" 
B)  "$\Omega$mass+$\Omega$ $\wedge$  = 1" 
C)  "$\Omega$mass +$\Omega$luminous = 1" 
D)  "$\Omega$luminous +$\Omega$ $\wedge$  = 1" 
E)  "$\Omega$luminous +$\Omega$ $\wedge$  = 0" 
A)  "$\Omega$mass + $\Omega$ $\wedge$  = 0" 
B)  "$\Omega$mass+$\Omega$ $\wedge$  = 1" 
C)  "$\Omega$mass +$\Omega$luminous = 1" 
D)  "$\Omega$luminous +$\Omega$ $\wedge$  = 1" 
E)  "$\Omega$luminous +$\Omega$ $\wedge$  = 0"

Question 8

What was the temperature of the universe when a typical CMB photon was no longer able to spontaneously create an electron and positron pair? Note that a photon has an energy equal to E = hc/$\lambda$, the CMB at any point in time has a blackbody spectrum that peaks at a wavelength $\lambda$peak = (2900$\mu$m K)/T, and the mass of a single electron is 9 * 10-31 kg.

Accepted Answer

A)  2000 K 
B)  400,000 K 
C)  2 million K 
D)  40 million K 
E)  2 billion K 
A)  2000 K 
B)  400,000 K 
C)  2 million K 
D)  40 million K 
E)  2 billion K

Question 9

The ratio of the average density in all forms of matter (luminous and dark) in our universe to the critical density is approximately 0.3.

Accepted Answer

A) True 
 B)False

Question 10

What can solve the flatness and horizon problem in cosmology, and why?

Accepted Answer

The concept of inflation in the very ear

Question 11

If  $\Omega$mass +  $\Omega$$\wedge$  = 1 today and dark energy were a cosmological constant, the universe would:

Accepted Answer

A)  expand forever 
B)  slow its expansion but never reverse it 
C)  stop expanding and eventually collapse 
D)  oscillate between expansion and collapse 
E)  expand so quickly that the universe is ripped apart 
A)  expand forever 
B)  slow its expansion but never reverse it 
C)  stop expanding and eventually collapse 
D)  oscillate between expansion and collapse 
E)  expand so quickly that the universe is ripped apart

Question 12

From the analysis of distant Type I supernovae and the Cosmic Microwave Background, we know that the Universe is approximately

Accepted Answer

A)  4.6 million years old 
B)  4.6 billion years old 
C)  6.5 thousand years old 
D)  13.7 million years old 
E)  13.7 billion years old 
A)  4.6 million years old 
B)  4.6 billion years old 
C)  6.5 thousand years old 
D)  13.7 million years old 
E)  13.7 billion years old

The fact that the currently observed $\Omega$ _mass + $\Omega$ _$\wedge$ is very close to 1 means that its value has always been very close to 1.

If you found a globular cluster that had an age of 20 billion years, what cosmological observations would conflict with this observation?

If there were no dark energy in the universe, the value of __________ would determine the evolution and fate of the universe.

To determine how the expansion rate of the universe has changed over time, astronomers directly measure the __________ for a sample of Type I supernovae in distant galaxies.

The concept of inflation helps solve both the problems of the flatness of the universe and smoothness of the cosmic background radiation.

As the universe cooled shortly after the Big Bang, which was the first fundamental force to separate itself out from the others?

The flatness problem arises because only a universe with __________ can have that value forever.

The ratio of the average density in all forms of matter (luminous and dark) in our universe to the critical density is approximately 0.3.

What can solve the flatness and horizon problem in cosmology, and why?

If $\Omega$ _mass + $\Omega$ _$\wedge$ = 1 today and dark energy were a cosmological constant, the universe would:

From the analysis of distant Type I supernovae and the Cosmic Microwave Background, we know that the Universe is approximately

Why Learn Astronomy

Patterns in the Skymotions of Earth

Motion of Astronomical Bodies

Gravity and Orbits

Light

The Tools of the Astronomer

The Birth and Evolution of Planetary Systems

The Terrestrial Planets and Earths Moon

Atmospheres of the Terrestrial Planets

Worlds of Gas and Liquid the Giant Planets

Planetary Adornmentsmoons and Rings

Dwarf Planets and Small Solar System Bodies

Taking the Measure of Stars

Our Starthe Sun

Star Formation and the Interstellar Medium

Evolution of Low-Mass Stars

Evolution of High-Mass Stars

Relativity and Black Holes

The Expanding Universe

Galaxies

The Milky Waya Normal Spiral Galaxy

Large-Scale Structure in the Universe

Life

Filters

Exam 22: Modern Cosmology

The fact that the currently observed Ω\OmegaΩ mass + Ω\OmegaΩ ∧\wedge∧ is very close to 1 means that its value has always been very close to 1.

If you found a globular cluster that had an age of 20 billion years, what cosmological observations would conflict with this observation?

If there were no dark energy in the universe, the value of __________ would determine the evolution and fate of the universe.

To determine how the expansion rate of the universe has changed over time, astronomers directly measure the __________ for a sample of Type I supernovae in distant galaxies.

The concept of inflation helps solve both the problems of the flatness of the universe and smoothness of the cosmic background radiation.

As the universe cooled shortly after the Big Bang, which was the first fundamental force to separate itself out from the others?

The flatness problem arises because only a universe with __________ can have that value forever.

The ratio of the average density in all forms of matter (luminous and dark) in our universe to the critical density is approximately 0.3.

What can solve the flatness and horizon problem in cosmology, and why?

If Ω\OmegaΩ mass + Ω\OmegaΩ ∧\wedge∧ = 1 today and dark energy were a cosmological constant, the universe would:

From the analysis of distant Type I supernovae and the Cosmic Microwave Background, we know that the Universe is approximately

Why Learn Astronomy

Patterns in the Skymotions of Earth

Motion of Astronomical Bodies

Gravity and Orbits

Light

The Tools of the Astronomer

The Birth and Evolution of Planetary Systems

The Terrestrial Planets and Earths Moon

Atmospheres of the Terrestrial Planets

Worlds of Gas and Liquid the Giant Planets

Planetary Adornmentsmoons and Rings

Dwarf Planets and Small Solar System Bodies

Taking the Measure of Stars

Our Starthe Sun

Star Formation and the Interstellar Medium

Evolution of Low-Mass Stars

Evolution of High-Mass Stars

Relativity and Black Holes

The Expanding Universe

Galaxies

The Milky Waya Normal Spiral Galaxy

Large-Scale Structure in the Universe

Life

Filters

The fact that the currently observed $\Omega$ _mass + $\Omega$ _$\wedge$ is very close to 1 means that its value has always been very close to 1.

If $\Omega$ _mass + $\Omega$ _$\wedge$ = 1 today and dark energy were a cosmological constant, the universe would: