The center of the Milky-Way lies in the direction of the constellation Cygnus. |
f |
The Milky Way is simiar in many ways to M31, the Andromeda Galaxy. |
t |
Our Sun lies about 30,000 light years out from the Galactic Center. |
t |
The Earth lies close to the center of the Galaxy. |
f |
The longer the period of pulsation for a Cepheid, the more massive and luminous the variable giant star is. |
t |
Because of their greater luminosity, RR Lyrae stars can be used at greater distances than can long-period Cepheids. |
f |
William Herschel’s original model for our Galaxy was based on counting stars. |
t |
Herschel’s original disk model placed us close to the center of the Galaxy. |
t |
Shapley’s measurements of the distances to open clusters vastly revised our understanding of our position in the Galaxy. |
t |
All Cepheids are giants, but not all giant stars are Cepheid variables. |
t |
Shapley found the globular cluster distribution equally concentrated all along the galactic plane. |
f |
Shapley found that globular clusters are only found in the Galactic bulge. |
f |
The problem with visual observations of our Galaxy is the luminous gas haze. |
f |
William Herschel made the first map of the Galaxy about 200 years ago. |
t |
The instability strip is above the main sequence on the H-R diagram. |
t |
RR Lyrae stars pulsate, but with shorter periods and lower luminosities than Cepheids. |
t |
The instability strip shows that not all main-sequence stars are, in face, stable. |
f |
It is harder to map the structure of the Milky Way in visible wavelengths than the radio and infrared waves. |
t |
All RR Lyrae stars are about 5 times the Sun’s luminosity. |
f |
All Cepheid variables discovered so far lie in other galaxies. |
f |
Like the RR Lyrae stars, Cepheids are all similar in luminosity, hence their use in measuring stellar distances. |
f |
Herschel believed teh Milky Way was a disk of stars, while Shapley found teh extended halo more like a ball. |
t |
Shapley found the globular clusters were strongly concentrated toward Sagittarius. |
t |
Harlow Shapley mapped the Milky Way using the period-luminosity relationship for RR Lyrae stars. |
t |
21 cm radio waves allow us to map the distribution of hydrogen in spiral arms on the opposite side of the Galaxy. |
t |
Population I stars came billions of years before Population II stars. |
f |
Cepheids are good examples of cataclysmic variable stars. |
f |
Halo stars are all Population II objects. |
t |
The orbit of the Solar System around the Galaxy is similar to that of a planet, almost circular and in the galactic plane. |
t |
Stars within an emission nebula, such as M42 are considered Population I stars. |
t |
The globular stars clusters are the most obvious examples of Population II around us. |
t |
The bright blue stars of Orion’s Belt are Population I, while our yellow Sun is population II. |
f |
Around us in the galactic plane, we find stars of a variety of ages and compositions. |
t |
The two stellar populations are extremes, but, in fact, stars with intermediate properties are common. |
t |
The thickness of the Galaxy near the Sun is about 1000 light years. |
t |
The orbits of Population II stars and globular clusters are much like comets, rising high above the galactic plane with eccentric orbits. |
t |
Planets are expected to be found orbiting most Population II stasr. |
f |
It would be very unlikely to find a massive young star out in the halo. |
t |
The rotation curve for our Galaxy shows stars beyond the Sun moving slower than expected. |
f |
The stars of the halo are all old, and those of the disk are all new. |
f |
Like our solar system, the whole Milky Way is about five billion years old. |
f |
The spiral arms are sites of continuous new star formation, accounting for their blue color and pink emission nebulae. |
t |
The density wave theory attempts to explain why the spiral arm structure persists over a long time. |
t |
Most of the dark matter in the Galaxy lies in the disk and galactic center. |
f |
The majority of the mass of the Milky Way lies farther out than the Sun’s orbit. |
t |
Dark matter has not been observed at any electromagnetic wavelength. |
t |
Most of the mass of our galaxy lies between Earth and the Galactic center. |
f |
Between us and the Galactic Center lie about 100 billion solar masses. |
t |
The core of the Milky Way, Sagittarius A, is a strong radio source in the sky. |
t |
Our surveys of the Galactic Center are better done in infrared than visible light. |
t |
The Sgr A* black hole may contain three million solar masses. |
t |
In structure, our Milky Way is most similar to |
c |
All RR Lyrae stars have about the same |
d |
The first attempt to map the Galaxy via star counts was done by |
b |
The RR Lyrae stars all have periods of |
c |
Which of the following are most massive and luminous? |
e |
A star in the instability strip of the H-R diagram would |
a |
For finding the distances to globular clusters, Harlow Shapley used |
d |
Why was Herschel’s strategy for mapping our Galaxy flawed? |
c |
Which of these variable stars would be classified as a RR Lyrae? |
b |
Which of these variable stars would be classified as a Cepheid? |
d |
The location of the Galactic Center was first found by Harlow Shapley with |
c |
Which is the correct description of the Sun’s location within the Milky Way? |
e |
The period-luminosity relation is critical in finding distances with |
d |
What is one of the differences between Cepheids and RR Lyrae variables? |
e |
Harlow Shapley found the Milky Way was |
d |
Which statement is true? |
b |
Which statement about Population II is false? |
d |
The orbits of Population II stars have been compared to |
c |
Galactic disks appear blue because |
d |
From the Sun, the distance to the Galactic Center is about |
b |
The Galactic Year is the time for our solar system to orbit the Galaxy; it is about |
b |
What is true about the stellar populations in the Galaxy? |
a |
Detailed measurements of the disk and central bulge region of our Galaxy suggest our Milky Way is a |
b |
Which of these objects have not been found in the Galactic Halo? |
c |
Between us and the Galactic Center, the Milky Way has a mass of |
d |
The tidal streams mapped in the Halo are similar to ______ in our solar system. |
b |
In our location in the Milky Way, the galactic disk is only about _____ light years thick. |
c |
Which of these is not typical of the Galaxy’s spiral arms? |
e |
In the formation of our Galaxy, the _____ formed first. |
c |
Which sequence of formation is most likely to be correct, oldest to youngest? |
b |
The visible color of the Galactic Bulge is |
b |
Most of the new star formation in the Galaxy is found in the |
b |
What use are 21 cm radio waves to galactic astronomers? |
c |
Density waves may explain |
d |
What two observations allow us to calculate mass of the portion of the Galaxy within the Sun’s orbit? |
c |
The dark halo is now believed to extend at least |
e |
What observations suggest the mass of the Galaxy goes much farther out than its visible disc? |
b |
Most of the mass of our Galaxy lies |
c |
Which method relies on the mass of a dark object revealing its presence? |
d |
Most of the mass of the MIlky Way seems to exist in the form of |
e |
At the center of our Galaxy lies |
b |
The radio source ______ is located in a place consistent with the center of our Galaxy. |
e |
The nearest comparable galaxy to our own lies in the constellation of _______. |
andromeda |
The center of the Milky Way lies in the direction of the constellation ______. |
sagittarius |
All globular cluster stars belong to Population _____. |
ii |
Based on his star counts, Herschel placed the Sun in the _____ of our Galaxy. |
center |
Herschel’s map of the Galaxy was too small because _____ blocked much of the starlight. |
dust |
To determine the distance to a Cepheid, we must measure its ______ of pulsation. |
period |
Edwin Hubble first found the distance to M21 in Andromeda with its _____ variable stars in its spiral arms. |
Cepheid |
Both RR Lyrae and Cepheid variables are giants that _____ in size over time. |
pulsate |
Optically mapping the Milky Way is made very difficult because of ______ in the disk. |
dust |
Star _____ have been vital in understanding stellar evolution, finding distances, and mapping the structure of our Galaxy. |
clusters |
Variable stars are ones whose _____ changes over time. |
luminosity |
It was _____ in the Galactic disk that threw Herschel’s model of the size and structure of the Galaxy off badly. |
dust |
This diagram shows the period-luminosity relationship. A Cepheid variable with a period of 5 days will have a luminosity of _____ solar luminosities. |
1000 |
The _____ variables in the closer globular clusters were used by Harlow Shapley to find their distances. |
rr lyrae |
The presence of _____ planets orbiting it shows us the Sun belongs to Population I. |
terrestrial |
If our Sun belonged to Population II, it is unlikely that _____ planets could orbit it. |
terrestrial |
William Herschel’s attempt to map our Galaxy was based on _____ in different directions in space. |
star counts |
Harvard woman astronomer ______ discovered the period-luminosity relation. |
henrietta leavitt |
Open clusters are found in the _____ of our Milky Way Galaxy. |
disc |
Our solar system lies in the galaxy’s ______, about 30,000 light years from the Galactic Center. |
disk |
Almost all the stars we see around us with the naked eye are relatively _____ in age. |
young |
Virtually the entire disk of the Galaxy has been mapped using the _____ wavelength. |
21 cm |
The three main components of the Milky Way galaxy are: |
disk, bulge, halo |
The spiral arms are made of bright stars belonging to Population ___. |
i |
Harlow Shapley found the visible disk of the Galaxy is about _____ kpc across. |
30 |
With respect to heavy elements, the stars of the Halo are _____ in metals. |
poor |
The spherical distribution of the globular clusters in the Halo reminds us of the similar distribution of cometary nuclei in the _____ cloud. |
oort |
The distribution of stars in the Galactic Bulge reminds us of the distribution of objects in the solar system’s _____ Belt beyond Neptune. |
kuiper |
The age of the whole Galaxy has been found from studies of its oldest stars in the ____ clusters that orbit in the Halo. |
globular |
The Galactic Disk has been flattened by the _____ of the Galaxy. |
rotation |
The distribution of Population II stars and globular clusters shows the Galaxy was more _____ in shape when it formed than it is now. |
spherical |
According to the ages of the globular clusters, our Galaxy is about _____ times as old as the solar system. |
two |
The _____ is the spherical outer portion of the Galaxy, including the orbits of the globular clusters and most dark matter. |
halo |
It is the distribution of _____ atoms in the spiral arms that is measured with 21 cm radio maps. |
hydrogen |
Most of the hot, young blue stars lie in the _____ of our Galaxy. |
spiral arms |
According to its rotation curve, the majority of our Galaxy’s mass is ______. |
dark amtter |
To the outer edge of the Galaxy, the rotation curve finds objects moving _____ than Kepler’s Laws would lead us to expect. |
faster |
We can estimate the mass of the Galaxy from observations of its _____ curve. |
rotation |
Counting only the material between us and the galactic Center, we measure a mass of _____ billion Suns. |
100 |
Most of the mass of the Galaxy lies in the _____. |
dark halo |
The bending of distant starlight by a closer object, resulting in a temporary brightening of the star, is called _____. |
gravitational lensing |
The strange object ____ is believed to be the black hole in the center of our Galaxy. |
sagittarius a |
Sagittarius A* was first noted due to its strong ____ emissions. |
radio |
What are the three main parts of our Galaxy? |
disk, bulge, halo |
Astronomy Ch. 14 Practice Test
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