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==AstroTest4_Study==
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===AstroTest4_Study-v1s1 ===
<div style="page-break-inside:avoid;">
 
1. <!--AstroStellarMeasurements_1-->Stellar parallax is 
 
:___ a) a numerical measure of brightness as seen from Earth
 
:___ b) an annual change in angular position of a star as seen from Earth
 
:___ c) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
:___ d) the total amount of energy emitted per unit time.
 
:___ e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
2. <!--AstroStellarMeasurements_2-->Luminosity is 
 
:___ a) the total amount of energy emitted per unit time.
 
:___ b) an annual change in angular position of a star as seen from Earth
 
:___ c) a numerical measure of brightness as seen from Earth
 
:___ d) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
:___ e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
3. <!--AstroStellarMeasurements_3-->A standard candle is
 
:___ a) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
:___ b) the total amount of energy emitted per unit time.
 
:___ c) an annual change in angular position of a star as seen from Earth
 
:___ d) a numerical measure of brightness as seen from Earth
 
:___ e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
4. <!--AstroStellarMeasurements_4-->Absolute magnitude is 
 
:___ a) an astronomical object with known luminosity.
 
:___ b) the total amount of energy emitted per unit time.
 
:___ c) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
:___ d) an annual change in angular position of a star as seen from Earth
 
:___ e) a numerical measure of brightness as seen from Earth
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
5. <!--AstroStellarMeasurements_5-->Relative magnitude is
 
:___ a) the total amount of energy emitted per unit time.
 
:___ b) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
:___ c) an astronomical object with known luminosity.
 
:___ d) a numerical measure of brightness as seen from Earth
 
:___ e) an annual change in angular position of a star as seen from Earth
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
6. <!--AstroStellarMeasurements_6-->In 1989 the satellite [[w:Hipparcos|Hipparcos]] was launched primarily for obtaining parallaxes and [[w:proper motion|proper motions]] allowing measurements of stellar parallax for stars up to about 500 parsecs away, which is about ____ times the diameter of the [[w:Milky_Way|Milky Way Galaxy]].
 
:___ a) 15
 
:___ b) 0.15
 
:___ c) .015
 
:___ d) 150
 
:___ e) 1.5
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
7. <!--AstroStellarMeasurements_7-->An object emits thermal (blackbody) radiation with a peak wavelength of 250nm.  How does its temperature compare with the Sun?  
 
:___ a)  2 times hotter than the Sun
 
:___ b) The temperature is the same
 
:___ c)  5 times hotter than the Sun
 
:___ d)  2 times colder than the Sun
 
:___ e)  5 times colder than the Sun 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
8. <!--AstroStellarMeasurements_8-->The "normalized intensity" of a Sun-like star situated one parsec from Earth would be 4&pi;I = 1.  What is 4&pi;I for a star with 100 times the Sun's energy output that is situated 10pc from Earth?
 
:___ a) 10<sup>-4</sup>
 
:___ b) 1
 
:___ c) 10<sup>-1</sup>
 
:___ d) 10<sup>-3</sup>
 
:___ e) 10<sup>-2</sup>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
9. <!--AstroStellarMeasurements_9-->An orbiting satellite makes a circular orbit 5 AU from the Sun.  It measures a parallax angle of 0.2 of an arcsecond (each way from the average position).  What is the star's distance? 
 
:___ a) 5 parsecs
 
:___ b) 1 parsec
 
:___ c) 25 parsecs
 
:___ d) 50 parsecs
 
:___ e) 10 parsecs
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
10. <!--AstroStellarMeasurements_10-->A star that is increasing it's temperature while maintaining constant luminosity is
 
:___ a) in the process of dying
 
:___ b) getting smaller in size
 
:___ c) turning red
 
:___ d) on the verge of becoming a supernovae
 
:___ e)e) getting larger in size
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
11. <!--AstroStellarMeasurements_11-->The range of wavelength for visible light is between
 
:___ a) 0.1 and 10 nanometers
 
:___ b) 600 and 1200 nanometers
 
:___ c) 5000 and 6000 nanometers
 
:___ d) 400 and 700 nanometers
 
:___ e) 1 and 10 nanometers
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
12. <!--AstroStellarMeasurements_12-->Based on the HR diagrams and images in stars shown in the materials, a very large red supergiant has a diameter that is about ____ greater than a small white dwarf.
 
:___ a) 3x10<sup>7</sup>
 
:___ b) 3x10<sup>5</sup>
 
:___ c) 3x10<sup>9</sup>
 
:___ d) 3x10<sup>11</sup>
 
:___ e) 3x10<sup>3</sup>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
13. <!--AstroWikipStar_1-->Why is a star made of plasma? 
 
:___ a) plasma is always present when there are strong magnetic fields
 
:___ b) it is so hot that electrons are stripped away from the protons 
 
:___ c) the interstellar gas was mostly plasma
 
:___ d) the intense gravity liquifies the substance, just as red blood cells liquify plasma in the body
 
:___ e) plasma is generic word for "important"
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
14. <!--AstroWikipStar_2-->What is the difference between a constellation and an asterism? 
 
:___ a) asterisms are smaller than constellations
 
:___ b) asterisms are larger than constellations
 
:___ c) none of these is correct
 
:___ d) constellations consist of never more than ten stars.
 
:___ e) constellations represent regions of the sky, like state boundaries on a map of the USA
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
15. <!--AstroWikipStar_3-->Stellar parallax is 
 
:___ a) Two of these is correct
 
:___ b) Using changes in the angular position of a star to deduce the star’s distance
 
:___ c) Triangulation to deduce the distance to nearby stars
 
:___ d) Using spectral lines to deduce the distance to nearby stars
 
:___ e) None of these is correct.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
16. <!--AstroWikipStar_4-->Giant molecular clouds with sufficient conditions to form a star cluster would have formed them long ago.  Any stellar births in the past couple of billions years probably resulted from _____ between clouds. 
 
:___ a) photon exchange
 
:___ b) None of these is correct.
 
:___ c) ion exchange
 
:___ d) Two of these are correct
 
:___ e) collisions 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
17. <!--AstroWikipStar_5-->A starburst galaxy. 
 
:___ a) has only dead or dying stars
 
:___ b) is a region of active stellar birth
 
:___ c) Two of these are correct
 
:___ d) usually is a result of collisions between galaxies 
 
:___ e) All of these are correct
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
18. <!--AstroWikipStar_6-->Which of the following expresses Jean's criterion for the collapse of a giant molecular cloud of mass, M, radius, R, and temperature T, and pressure P? (Here ?  is some constant) 
 
:___ a) P>?MR 
 
:___ b) T>?RM
 
:___ c) M>?RT
 
:___ d) R>?MT
 
:___ e) P>?MT
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
19. <!--AstroWikipStar_7-->Which of the following changes in the properties of a giant molecular cloud might cause it to collapse? 
 
:___ a) Two of these are correct
 
:___ b) Increase mass at fixed temperature and size
 
:___ c) Decrease mass at fixed temperature and size
 
:___ d) Increase size at fixed pressure and mass
 
:___ e) Increase temperature at fixed mass and size
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
20. <!--AstroWikipStar_8-->What happens if you increase the size of a giant molecular cloud while keeping temperature and mass fixed? 
 
:___ a) It is equally likely to collapse because size is not part of the Jean's criterion.
 
:___ b) It is less likely to collapse because temperature can never be kept fixed
 
:___ c) It is more likely to collapse because this will increase the temperature
 
:___ d) It is more likely to collapse because larger things have more gravity
 
:___ e) It is less likely to collapse spreading it out weakens the force of gravity
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
21. <!--AstroWikipStar_9-->What is a Bok globule in the formation of stellar systems? 
 
:___ a) A black hole that enters a cloud and triggers the collapse
 
:___ b) A cluster of giant molecular clouds that coalesce to form a solar system
 
:___ c) A small portion of a giant cloud that collapses
 
:___ d) A supernovae precurser that attracts more gas atoms
 
:___ e) A small planet that formed before any stars have formed
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
22. <!--AstroWikipStar_10-->Pre–main sequence stars are often surrounded by a protoplanetary disk and powered mainly by  
 
:___ a) the fission of Carbon from Helium
 
:___ b) collisions between protoplanets
 
:___ c) the release of gravitational energy
 
:___ d) chemical reactions
 
:___ e) the fusion of Helium to Carbon
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
23. <!--AstroWikipStar_11-->Stars that begin with more than 50 solar masses will typically lose _______ while on the main sequence. 
 
:___ a) all of their magnetic field
 
:___ b) 10% their mass
 
:___ c) 1%  their mass
 
:___ d) 10% of their magnetic field
 
:___ e) 50% their mass 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
24. <!--AstroWikipStar_12-->The Hayashi and Henyey tracks refer to how T Tauri of different masses will move 
 
:___ a) through a cluster as they die
 
:___ b) through an HR diagram as they die
 
:___ c) through an HR diagram as they are born
 
:___ d) through a cluster as they are born
 
:___ e) Two of these are true 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
25. <!--AstroWikipStar_13-->How do low-mass stars change as they are born?[[File:PMS evolution tracks.svg|thumb|Birth of stars HR path tracks]]  
 
:___ a) Decreasing luminosity with no change in temperature
 
:___ b) Decreasing temperature with no change in luminosity
 
:___ c) Decreasing temperature and increasing luminosity
 
:___ d) Increasing temperature with no change in luminosity
 
:___ e) Increasing luminosity with no change in temperature
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
26. <!--AstroWikipStar_14-->When a star with more than 10 solar masses ceases fuse hydrogen to helium, it 
 
:___ a) it fuses helium to carbon and other elements up to iron and then ceases to produce more energy
 
:___ b) it fuses elements up to uranium, and continues to produce energy by the fission of uranium.
 
:___ c) it fuses helium to carbon and then ceases to produce more energy
 
:___ d) ceases to convert nuclear energy.
 
:___ e) it fuses helium to carbon to iron (and other elements), then continues to release more energy by fusing the iron to heavier elements such as uranium.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
27. <!--AstroWikipStar_15-->Many supernovae begin as a shock wave in the core that was caused by 
 
:___ a) all of these processes contribute to the shock wave
 
:___ b) iron fusing into heavier elements such as uranium
 
:___ c) the conversion of carbon into diamonds, 
 
:___ d) carbon and other elements fusing into iron
 
:___ e) electrons being driven into protons to form neutrons
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
28. <!--AstroWikipStar_16-->A dying star with more than 1.4 solar masses becomes a ______, and those with more than 5 solar masses becomes a _____ 
 
:___ a) blue giant....red giant
 
:___ b) white dwarf....neutron star
 
:___ c) white dwarf....black hole
 
:___ d) neutron star....black hole
 
:___ e) white dwarf...red dwarf
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
29. <!--AstroWikipStar_17-->According to Wikipedia, a star with over 20 solar masses converts its Hyrogen to Helium in about 8 billion years, but the conversion of Oxygen to heavier elements take about _____  
 
:___ a) 1 million years
 
:___ b) 1 billion years
 
:___ c) 1 thousand years
 
:___ d) 1 year
 
:___ e) 10 billion years
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
30. <!--AstroStarCluster_1-->A grouping with 100 thousand stars would probably be a
 
:___ a)  elliptical galaxy
 
:___ b)  A-B association
 
:___ c)  dwarf galaxy
 
:___ d)  open cluster
 
:___ e)  globular cluster
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
31. <!--AstroStarCluster_2-->A grouping with a hundred stars is probably a
 
:___ a)  globular cluster
 
:___ b)  A-B association
 
:___ c)  elliptical galaxy
 
:___ d)  dwarf galaxy
 
:___ e)  open cluster
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
32. <!--AstroStarCluster_3-->I gravity is what holds stars in a cluster together, what is the most important process that causes them to spread apart?
 
:___ a)  anti-gravity
 
:___ b)  supernovae
 
:___ c)  magnetism
 
:___ d)  random motion
 
:___ e)  solar wind
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
33. <!--AstroStarCluster_4-->Members of an open cluster feel significant forces only due to gravitational interaction with each other
 
:___ a)  True
 
:___ b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
34. <!--AstroStarCluster_5-->Members of an open cluster feel significant forces from nearby giant molecular clouds
 
:___ a)  True
 
:___ b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
35. <!--AstroStarCluster_6-->Members of a globular cluster tend to be
 
:___ a)  of all ages
 
:___ b)  old
 
:___ c)  young
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
36. <!--AstroStarCluster_7-->Members of a globular cluster tend to have
 
:___ a)  a wide range of masses
 
:___ b)  low mass
 
:___ c)  high mass
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
37. <!--AstroStarCluster_8-->In 1917, the astronomer Harlow Shapley was able to estimate the Sun's distance from the galactic centre using
 
:___ a)  goblular clusters
 
:___ b)  a combination of open and globular clusters
 
:___ c)  open clusters
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
38. <!--AstroStarCluster_9-->Most globular clusters that we see in the sky orbit _____ and have ______ orbits
 
:___ a)  within the disk of the Milky way ... nearly circular
 
:___ b)  within the disk of the Milky way ... elliptic orbits
 
:___ c)  the center of the Milky way ... nearly circular
 
:___ d)  the center of the Milky way ... elliptic orbits
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
39. <!--AstroStarCluster_10-->Many stars in a typical open cluster are nearly as old as the universe
 
:___ a)  True
 
:___ b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
40. <!--AstroStarCluster_11-->Many stars in a typical globular cluster are nearly as old as the universe
 
:___ a)  True
 
:___ b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
41. <!--AstroStarCluster_12-->The number of globular clusters in the Milky way galaxy is about
 
:___ a)  15 thousand
 
:___ b)  1,500
 
:___ c)  15 million
 
:___ d)  150
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
42. <!--AstroStarCluster_13-->The location of open clusters can be described as
 
:___ a)  uniformly distributed within the galactic disk
 
:___ b)  uniformly distributed in a sphere centered at the Milky Way's center
 
:___ c)  between the spiral arms
 
:___ d)  in the spiral arms
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
43. <!--AstroStarCluster_14-->Stars can "evaporate" from a cluster.  What does this mean?
 
:___ a)  Close encounters between 3 or more cluster members gives one star enough speed to leave the cluster
 
:___ b)  The gravitational attraction between stars evaporates the gas from stars
 
:___ c)  The solar wind from neighboring stars blows the atmosphere away
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
44. <!--AstroSizeWhitdwrfNeutstarQSO_1-->At the center of the Crab nebula is 
 
:___ a)b) a pulsar
 
:___ b)e) the remnants of a supernova
 
:___ c)a) all of these is correct
 
:___ d)d) a neutron star
 
:___ e)c) none of these is correct
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
45. <!--AstroSizeWhitdwrfNeutstarQSO_2-->Aside from its location on the HR diagram, evidence that the white dwarf has a small radius can be found from
 
:___ a) the temperature
 
:___ b) the mass as measured by Kepler's third law (modified by Newton)
 
:___ c) the expansion of the universe
 
:___ d) the doppler shift
 
:___ e) the gravitational redshift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
46. <!--AstroSizeWhitdwrfNeutstarQSO_3-->[[Image:A0V-blackbody SPD comparison.png|240px|right]]<br><br>This spectrum of the star Vega suggests that
 
:___ a) it can be associated with an "effective" temperature
 
:___ b) if is not really a black body
 
:___ c) it's surface can be associated with a range of temperatures
 
:___ d) all of these are true
 
:___ e) it is an approximate black body
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
47. <!--AstroSizeWhitdwrfNeutstarQSO_4-->Which of the following is NOT an essential piece of a a strong argument that a white dwarf is not only the size of the earth, but typically has the same mass as the Sun. 
 
:___ a) the distance to Sirius A
 
:___ b) all of these are true
 
:___ c) the wobble of Sirius A
 
:___ d) the relative magnitude of Sirius B
 
:___ e) the "color" (spectral class) of Sirius B
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
48. <!--AstroSizeWhitdwrfNeutstarQSO_5-->The course materials presented three arguments suggesting that a white dwarf is roughly the size of the earth.  Which best summarizes them?
 
:___ a) doppler-shift...period-of-pulsation...temperature-luminosity
 
:___ b) temperature-luminosity...redshift...quantum-theory-of-solids
 
:___ c) x-ray-emmission...doppler-shift...rotation-rate
 
:___ d) all of these are true
 
:___ e) HR-diagram-location...X-ray-emmision...spectral-lines
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
49. <!--AstroSizeWhitdwrfNeutstarQSO_6-->As of 2008, the percent uncertainty in the distance to the Crab nebula is approximately, 
 
:___ a) 0.1%
 
:___ b) 10%
 
:___ c) 100%
 
:___ d) 25%
 
:___ e) 1%
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
50. <!--AstroSizeWhitdwrfNeutstarQSO_7-->What was Messier doing when he independently rediscovered the Crab in 1758? 
 
:___ a) Attempting to count asteroids
 
:___ b) Looking for lobsters
 
:___ c) Attempting one of the first star charts
 
:___ d) Looking for a comet that he knew would be appearing in that part of the sky.
 
:___ e) Trying to measure the orbital radius of a planet
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
51. <!--AstroSizeWhitdwrfNeutstarQSO_8-->[[File:Gravitational red-shifting2.png|thumb|180px]]<br><br>What best explains this figure?
 
:___ a) The photon slows down as it goes uphill, and by c=f&lambda; it increases wavelength therefore by E=hf, it turns red.
 
:___ b) The photon slows down, by the Doppler shift, c=f&lambda;, and therefore by  E=hf it turns red.
 
:___ c) The photon loses energy, not speed.  By c=f&lambda; , it loses frequency, and by E=hf it increases wavelength and turns red.
 
:___ d) The photon slows down, by the Doppler shift, E=hf, and therefore by c=f&;lambda it turns red.
 
:___ e) The photon loses energy, not speed.  By E=hf, it loses frequency, and by c=f&lambda; it increases wavelength and turns red.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
52. <!--AstroSizeWhitdwrfNeutstarQSO_9-->What causes the blue glow of the Crab nebula?
 
:___ a) the same emission found in a Lava lamp (ultra-violet)
 
:___ b) the curving motion of electrons in a magnetic field; such motion traps ultra-violet and blue light
 
:___ c) the curving motion of electrons in a magnetic field; such motion resembles a radio antenna
 
:___ d) the Doppler blue shift
 
:___ e) the Gravitational blue shift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
53. <!--AstroSizeWhitdwrfNeutstarQSO_10-->One way to determine the distance to a nebula or small cluster of clouds is to compare the angular expansion to the spectroscopic Doppler shift.  Two clusters (A and B) have the same spectroscopically measured velocity.  Cluster A is moving towards the observer and exhibits the greater angular expansion.  Which cluster is closer? 
 
:___ a) cluster B, because it exhibits less angular expansion
 
:___ b) either cluster might be more distant
 
:___ c) cluster A, because it exhibits greater angular expansion
 
:___ d) cluster B, because it exhibits a red Doppler shift
 
:___ e) cluster A, because it exhibits a blue Doppler shift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
54. <!--AstroSizeWhitdwrfNeutstarQSO_11-->What causes the "finger-like" filamentary structure in the Crab nebula?
 
:___ a) cyclotron motion, causing the electrons to strike oxygen molecules
 
:___ b) electrons striking hydrogen molecules, like a lava lamp
 
:___ c) a light(low density) fluid underneath a heavy(high density) fluid, like a lava lamp
 
:___ d) electrons striking oxygen molecules, like a lava lamp
 
:___ e) a heavy (high density) fluid underneath a light (low density) fluid, like a lava lamp
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
55. <!--AstroSizeWhitdwrfNeutstarQSO_12--><math>KE=\frac{4\pi^2}{5}\frac{MR^2}{P^2}</math> is the kinetic energy of a solid rotating ball, where M is mass, R is radius, and P is period. And, <math>power=\frac{energy}{time}</math>.<br>You are banging espressos in a little coffeehouse with your astronomy friends, talking about a new SN remnant that closely resembles the Crab.  You have observed the pulsar, and wonder what the total power output of the nebula might be.  You know both the period of the pulsar, as well as <math>\tau</math>, which represents the amount of time you think the pulsar will continue pulsing if it continues slowing down at its present rate.  What formula do you write on your napkin?
 
:___ a) <math>power=\frac{4\pi^2}{5\tau}\frac{MR^2}{P^2}</math>
 
:___ b) <math>power=\frac{4\tau\pi^2}{5}\frac{MR^2}{P^2}</math>
 
:___ c) <math>power=\frac{5}{4\tau\pi^2}\frac{MR^2}{P^2}</math>
 
:___ d) <math>power=\frac{4\pi^2}{5\tau^2}\frac{MR^2}{P^2}</math>
 
:___ e) <math>power=\frac{4\pi^2}{5}\frac{MR^2}{P^2}\tau^4</math>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
56. <!--AstroSizeWhitdwrfNeutstarQSO_13-->In one respect, the universie is arguably "young", considering how much complexity it contains.  This is often illustrated by a calculation of
 
:___ a) recalibration of supernovae luminosity
 
:___ b) cosmic expansion
 
:___ c) cosmic redshift
 
:___ d) chimps typing Shakespeare
 
:___ e) recalibration of supernovae relative magnitude
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
57. <!--AstroSizeWhitdwrfNeutstarQSO_14-->Comparing Hubble's original (1929) plot of redshift versus distance with the later one in 2007, the latter extends farther into space by a factor of
 
:___ a) 100
 
:___ b) 100,000
 
:___ c) 10,000
 
:___ d) 10
 
:___ e) 1000
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
58. <!--AstroSizeWhitdwrfNeutstarQSO_15-->The course materials present two cosmic expansion plots.   Hubble's original (1929) plot used
 
:___ a) Cepheid variables
 
:___ b) novae
 
:___ c) entire galaxies
 
:___ d) supernovae
 
:___ e) red giants
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
59. <!--AstroSizeWhitdwrfNeutstarQSO_16-->The course materials present two cosmic expansion plots.   The more recent (2007) plot used
 
:___ a) red giants
 
:___ b) supernovae
 
:___ c) Cepheid variables
 
:___ d) novae
 
:___ e) entire galaxies
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
60. <!--AstroSizeWhitdwrfNeutstarQSO_17-->Place yourself in an expanding raisinbread model of Hubble expansion.  A raisin originally situated at a distance of 4 cm expands out to 12 cm.  To what distance would a raisin originally situated at a distance of 2 cm expand?
 
:___ a) 2
 
:___ b) 6
 
:___ c) 8
 
:___ d) 3
 
:___ e) 4
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
61. <!--AstroSizeWhitdwrfNeutstarQSO_18-->You at the center raisin of an expanding raisinbread model of Hubble expansion, and from your location a raisin originally situated at a distance of 1 cm expands out to a distance of 4 cm.  The nearest raisin with intelligent life is situated exactly halfway between your (central) location and the edge.  How would this second "intelligent" raisin view an expansion of a raisin 1 cm away?
 
:___ a) expansion from 1 cm to 2 cm (half of yours)
 
:___ b) expansion from 1 cm to 3 cm (since 3-1=2)
 
:___ c) expansion from 1 cm to 8 cm (twice yours).
 
:___ d) expansion from 1 cm to 9 cm (since 5-1=4)
 
:___ e) expansion from 1 cm to 4 cm (just like yours).
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
62. <!--AstroSizeWhitdwrfNeutstarQSO_19-->Place yourself in an expanding raisinbread model of Hubble expansion.  A raisin originally situated at a distance of 2 cm expands out to 4 cm.  To what distance would a raisin originally situated at a distance of 4 cm expand?
 
:___ a) 8
 
:___ b) 6
 
:___ c) 2
 
:___ d) 3
 
:___ e) 4
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
63. <!--AstroSizeWhitdwrfNeutstarQSO_20-->[[File:Light-clock.png|thumb]]This light clock is associated with 
 
:___ a) all of these are true
 
:___ b) doppler shift
 
:___ c) gravitational shift
 
:___ d) general relativity
 
:___ e) special relativity
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
64. <!--AstroSizeWhitdwrfNeutstarQSO_21-->[[File:Light-clock.png|thumb]]Suppose the light clock involved a ball being tossed back and forth on a train going just under the speed of sound.  In contrast to the situation for light reflecting back and forth on a train going just under the speed of light, there is virtually no time dilation.  Why?
 
:___ a) Special relativity is valid only for objects travelling in a vacuum.
 
:___ b) The observer on the ground would perceive the ball to be travelling faster.
 
:___ c) The observer on the ground would perceive the width the train to be greater.
 
:___ d) The observer on the ground would perceive the ball to be travelling more slowly.
 
:___ e) The observer on the ground would perceive the width the train to be smaller.
 
</div>
 
 
{{pagebreak}}
 
==== Key to  AstroTest4_Study-v1s1 ====
 
<div style="page-break-inside:avoid;">
 
1. <!--AstroStellarMeasurements_1-->Stellar parallax is 
 
::  - a) a numerical measure of brightness as seen from Earth
 
::  + b) an annual change in angular position of a star as seen from Earth
 
::  - c) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
::  - d) the total amount of energy emitted per unit time.
 
::  - e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
2. <!--AstroStellarMeasurements_2-->Luminosity is 
 
::  + a) the total amount of energy emitted per unit time.
 
::  - b) an annual change in angular position of a star as seen from Earth
 
::  - c) a numerical measure of brightness as seen from Earth
 
::  - d) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
::  - e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
3. <!--AstroStellarMeasurements_3-->A standard candle is
 
::  - a) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
::  - b) the total amount of energy emitted per unit time.
 
::  - c) an annual change in angular position of a star as seen from Earth
 
::  - d) a numerical measure of brightness as seen from Earth
 
::  + e) an astronomical object with known luminosity.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
4. <!--AstroStellarMeasurements_4-->Absolute magnitude is 
 
::  - a) an astronomical object with known luminosity.
 
::  - b) the total amount of energy emitted per unit time.
 
::  + c) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
::  - d) an annual change in angular position of a star as seen from Earth
 
::  - e) a numerical measure of brightness as seen from Earth
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
5. <!--AstroStellarMeasurements_5-->Relative magnitude is
 
::  - a) the total amount of energy emitted per unit time.
 
::  - b) a numerical measure of brightness as seen from a distance of approximately 33 light-years
 
::  - c) an astronomical object with known luminosity.
 
::  + d) a numerical measure of brightness as seen from Earth
 
::  - e) an annual change in angular position of a star as seen from Earth
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
6. <!--AstroStellarMeasurements_6-->In 1989 the satellite [[w:Hipparcos|Hipparcos]] was launched primarily for obtaining parallaxes and [[w:proper motion|proper motions]] allowing measurements of stellar parallax for stars up to about 500 parsecs away, which is about ____ times the diameter of the [[w:Milky_Way|Milky Way Galaxy]].
 
::  - a) 15
 
::  - b) 0.15
 
::  + c) .015
 
::  - d) 150
 
::  - e) 1.5
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
7. <!--AstroStellarMeasurements_7-->An object emits thermal (blackbody) radiation with a peak wavelength of 250nm.  How does its temperature compare with the Sun?  
 
::  + a)  2 times hotter than the Sun
 
::  - b) The temperature is the same
 
::  - c)  5 times hotter than the Sun
 
::  - d)  2 times colder than the Sun
 
::  - e)  5 times colder than the Sun 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
8. <!--AstroStellarMeasurements_8-->The "normalized intensity" of a Sun-like star situated one parsec from Earth would be 4&pi;I = 1.  What is 4&pi;I for a star with 100 times the Sun's energy output that is situated 10pc from Earth?
 
::  - a) 10<sup>-4</sup>
 
::  + b) 1
 
::  - c) 10<sup>-1</sup>
 
::  - d) 10<sup>-3</sup>
 
::  - e) 10<sup>-2</sup>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
9. <!--AstroStellarMeasurements_9-->An orbiting satellite makes a circular orbit 5 AU from the Sun.  It measures a parallax angle of 0.2 of an arcsecond (each way from the average position).  What is the star's distance? 
 
::  - a) 5 parsecs
 
::  - b) 1 parsec
 
::  + c) 25 parsecs
 
::  - d) 50 parsecs
 
::  - e) 10 parsecs
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
10. <!--AstroStellarMeasurements_10-->A star that is increasing it's temperature while maintaining constant luminosity is
 
::  - a) in the process of dying
 
::  + b) getting smaller in size
 
::  - c) turning red
 
::  - d) on the verge of becoming a supernovae
 
::  - e)e) getting larger in size
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
11. <!--AstroStellarMeasurements_11-->The range of wavelength for visible light is between
 
::  - a) 0.1 and 10 nanometers
 
::  - b) 600 and 1200 nanometers
 
::  - c) 5000 and 6000 nanometers
 
::  + d) 400 and 700 nanometers
 
::  - e) 1 and 10 nanometers
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
12. <!--AstroStellarMeasurements_12-->Based on the HR diagrams and images in stars shown in the materials, a very large red supergiant has a diameter that is about ____ greater than a small white dwarf.
 
::  - a) 3x10<sup>7</sup>
 
::  + b) 3x10<sup>5</sup>
 
::  - c) 3x10<sup>9</sup>
 
::  - d) 3x10<sup>11</sup>
 
::  - e) 3x10<sup>3</sup>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
13. <!--AstroWikipStar_1-->Why is a star made of plasma? 
 
::  - a) plasma is always present when there are strong magnetic fields
 
::  + b) it is so hot that electrons are stripped away from the protons 
 
::  - c) the interstellar gas was mostly plasma
 
::  - d) the intense gravity liquifies the substance, just as red blood cells liquify plasma in the body
 
::  - e) plasma is generic word for "important"
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
14. <!--AstroWikipStar_2-->What is the difference between a constellation and an asterism? 
 
::  - a) asterisms are smaller than constellations
 
::  - b) asterisms are larger than constellations
 
::  - c) none of these is correct
 
::  - d) constellations consist of never more than ten stars.
 
::  + e) constellations represent regions of the sky, like state boundaries on a map of the USA
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
15. <!--AstroWikipStar_3-->Stellar parallax is 
 
::  + a) Two of these is correct
 
::  - b) Using changes in the angular position of a star to deduce the star’s distance
 
::  - c) Triangulation to deduce the distance to nearby stars
 
::  - d) Using spectral lines to deduce the distance to nearby stars
 
::  - e) None of these is correct.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
16. <!--AstroWikipStar_4-->Giant molecular clouds with sufficient conditions to form a star cluster would have formed them long ago.  Any stellar births in the past couple of billions years probably resulted from _____ between clouds. 
 
::  - a) photon exchange
 
::  - b) None of these is correct.
 
::  - c) ion exchange
 
::  - d) Two of these are correct
 
::  + e) collisions 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
17. <!--AstroWikipStar_5-->A starburst galaxy. 
 
::  - a) has only dead or dying stars
 
::  - b) is a region of active stellar birth
 
::  + c) Two of these are correct
 
::  - d) usually is a result of collisions between galaxies 
 
::  - e) All of these are correct
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
18. <!--AstroWikipStar_6-->Which of the following expresses Jean's criterion for the collapse of a giant molecular cloud of mass, M, radius, R, and temperature T, and pressure P? (Here ?  is some constant) 
 
::  - a) P>?MR 
 
::  - b) T>?RM
 
::  + c) M>?RT
 
::  - d) R>?MT
 
::  - e) P>?MT
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
19. <!--AstroWikipStar_7-->Which of the following changes in the properties of a giant molecular cloud might cause it to collapse? 
 
::  - a) Two of these are correct
 
::  + b) Increase mass at fixed temperature and size
 
::  - c) Decrease mass at fixed temperature and size
 
::  - d) Increase size at fixed pressure and mass
 
::  - e) Increase temperature at fixed mass and size
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
20. <!--AstroWikipStar_8-->What happens if you increase the size of a giant molecular cloud while keeping temperature and mass fixed? 
 
::  - a) It is equally likely to collapse because size is not part of the Jean's criterion.
 
::  - b) It is less likely to collapse because temperature can never be kept fixed
 
::  - c) It is more likely to collapse because this will increase the temperature
 
::  - d) It is more likely to collapse because larger things have more gravity
 
::  + e) It is less likely to collapse spreading it out weakens the force of gravity
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
21. <!--AstroWikipStar_9-->What is a Bok globule in the formation of stellar systems? 
 
::  - a) A black hole that enters a cloud and triggers the collapse
 
::  - b) A cluster of giant molecular clouds that coalesce to form a solar system
 
::  + c) A small portion of a giant cloud that collapses
 
::  - d) A supernovae precurser that attracts more gas atoms
 
::  - e) A small planet that formed before any stars have formed
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
22. <!--AstroWikipStar_10-->Pre–main sequence stars are often surrounded by a protoplanetary disk and powered mainly by  
 
::  - a) the fission of Carbon from Helium
 
::  - b) collisions between protoplanets
 
::  + c) the release of gravitational energy
 
::  - d) chemical reactions
 
::  - e) the fusion of Helium to Carbon
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
23. <!--AstroWikipStar_11-->Stars that begin with more than 50 solar masses will typically lose _______ while on the main sequence. 
 
::  - a) all of their magnetic field
 
::  - b) 10% their mass
 
::  - c) 1%  their mass
 
::  - d) 10% of their magnetic field
 
::  + e) 50% their mass 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
24. <!--AstroWikipStar_12-->The Hayashi and Henyey tracks refer to how T Tauri of different masses will move 
 
::  - a) through a cluster as they die
 
::  - b) through an HR diagram as they die
 
::  + c) through an HR diagram as they are born
 
::  - d) through a cluster as they are born
 
::  - e) Two of these are true 
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
25. <!--AstroWikipStar_13-->How do low-mass stars change as they are born?[[File:PMS evolution tracks.svg|thumb|Birth of stars HR path tracks]]  
 
::  + a) Decreasing luminosity with no change in temperature
 
::  - b) Decreasing temperature with no change in luminosity
 
::  - c) Decreasing temperature and increasing luminosity
 
::  - d) Increasing temperature with no change in luminosity
 
::  - e) Increasing luminosity with no change in temperature
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
26. <!--AstroWikipStar_14-->When a star with more than 10 solar masses ceases fuse hydrogen to helium, it 
 
::  + a) it fuses helium to carbon and other elements up to iron and then ceases to produce more energy
 
::  - b) it fuses elements up to uranium, and continues to produce energy by the fission of uranium.
 
::  - c) it fuses helium to carbon and then ceases to produce more energy
 
::  - d) ceases to convert nuclear energy.
 
::  - e) it fuses helium to carbon to iron (and other elements), then continues to release more energy by fusing the iron to heavier elements such as uranium.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
27. <!--AstroWikipStar_15-->Many supernovae begin as a shock wave in the core that was caused by 
 
::  - a) all of these processes contribute to the shock wave
 
::  - b) iron fusing into heavier elements such as uranium
 
::  - c) the conversion of carbon into diamonds, 
 
::  - d) carbon and other elements fusing into iron
 
::  + e) electrons being driven into protons to form neutrons
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
28. <!--AstroWikipStar_16-->A dying star with more than 1.4 solar masses becomes a ______, and those with more than 5 solar masses becomes a _____ 
 
::  - a) blue giant....red giant
 
::  - b) white dwarf....neutron star
 
::  - c) white dwarf....black hole
 
::  + d) neutron star....black hole
 
::  - e) white dwarf...red dwarf
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
29. <!--AstroWikipStar_17-->According to Wikipedia, a star with over 20 solar masses converts its Hyrogen to Helium in about 8 billion years, but the conversion of Oxygen to heavier elements take about _____  
 
::  - a) 1 million years
 
::  - b) 1 billion years
 
::  - c) 1 thousand years
 
::  + d) 1 year
 
::  - e) 10 billion years
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
30. <!--AstroStarCluster_1-->A grouping with 100 thousand stars would probably be a
 
::  - a)  elliptical galaxy
 
::  - b)  A-B association
 
::  - c)  dwarf galaxy
 
::  - d)  open cluster
 
::  + e)  globular cluster
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
31. <!--AstroStarCluster_2-->A grouping with a hundred stars is probably a
 
::  - a)  globular cluster
 
::  - b)  A-B association
 
::  - c)  elliptical galaxy
 
::  - d)  dwarf galaxy
 
::  + e)  open cluster
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
32. <!--AstroStarCluster_3-->I gravity is what holds stars in a cluster together, what is the most important process that causes them to spread apart?
 
::  - a)  anti-gravity
 
::  - b)  supernovae
 
::  - c)  magnetism
 
::  + d)  random motion
 
::  - e)  solar wind
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
33. <!--AstroStarCluster_4-->Members of an open cluster feel significant forces only due to gravitational interaction with each other
 
::  - a)  True
 
::  + b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
34. <!--AstroStarCluster_5-->Members of an open cluster feel significant forces from nearby giant molecular clouds
 
::  + a)  True
 
::  - b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
35. <!--AstroStarCluster_6-->Members of a globular cluster tend to be
 
::  - a)  of all ages
 
::  + b)  old
 
::  - c)  young
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
36. <!--AstroStarCluster_7-->Members of a globular cluster tend to have
 
::  - a)  a wide range of masses
 
::  + b)  low mass
 
::  - c)  high mass
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
37. <!--AstroStarCluster_8-->In 1917, the astronomer Harlow Shapley was able to estimate the Sun's distance from the galactic centre using
 
::  + a)  goblular clusters
 
::  - b)  a combination of open and globular clusters
 
::  - c)  open clusters
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
38. <!--AstroStarCluster_9-->Most globular clusters that we see in the sky orbit _____ and have ______ orbits
 
::  - a)  within the disk of the Milky way ... nearly circular
 
::  - b)  within the disk of the Milky way ... elliptic orbits
 
::  - c)  the center of the Milky way ... nearly circular
 
::  + d)  the center of the Milky way ... elliptic orbits
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
39. <!--AstroStarCluster_10-->Many stars in a typical open cluster are nearly as old as the universe
 
::  - a)  True
 
::  + b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
40. <!--AstroStarCluster_11-->Many stars in a typical globular cluster are nearly as old as the universe
 
::  + a)  True
 
::  - b)  False
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
41. <!--AstroStarCluster_12-->The number of globular clusters in the Milky way galaxy is about
 
::  - a)  15 thousand
 
::  - b)  1,500
 
::  - c)  15 million
 
::  + d)  150
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
42. <!--AstroStarCluster_13-->The location of open clusters can be described as
 
::  - a)  uniformly distributed within the galactic disk
 
::  - b)  uniformly distributed in a sphere centered at the Milky Way's center
 
::  - c)  between the spiral arms
 
::  + d)  in the spiral arms
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
43. <!--AstroStarCluster_14-->Stars can "evaporate" from a cluster.  What does this mean?
 
::  + a)  Close encounters between 3 or more cluster members gives one star enough speed to leave the cluster
 
::  - b)  The gravitational attraction between stars evaporates the gas from stars
 
::  - c)  The solar wind from neighboring stars blows the atmosphere away
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
44. <!--AstroSizeWhitdwrfNeutstarQSO_1-->At the center of the Crab nebula is 
 
::  - a)b) a pulsar
 
::  - b)e) the remnants of a supernova
 
::  + c)a) all of these is correct
 
::  - d)d) a neutron star
 
::  - e)c) none of these is correct
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
45. <!--AstroSizeWhitdwrfNeutstarQSO_2-->Aside from its location on the HR diagram, evidence that the white dwarf has a small radius can be found from
 
::  - a) the temperature
 
::  - b) the mass as measured by Kepler's third law (modified by Newton)
 
::  - c) the expansion of the universe
 
::  - d) the doppler shift
 
::  + e) the gravitational redshift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
46. <!--AstroSizeWhitdwrfNeutstarQSO_3-->[[Image:A0V-blackbody SPD comparison.png|240px|right]]<br><br>This spectrum of the star Vega suggests that
 
::  - a) it can be associated with an "effective" temperature
 
::  - b) if is not really a black body
 
::  - c) it's surface can be associated with a range of temperatures
 
::  + d) all of these are true
 
::  - e) it is an approximate black body
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
47. <!--AstroSizeWhitdwrfNeutstarQSO_4-->Which of the following is NOT an essential piece of a a strong argument that a white dwarf is not only the size of the earth, but typically has the same mass as the Sun. 
 
::  - a) the distance to Sirius A
 
::  + b) all of these are true
 
::  - c) the wobble of Sirius A
 
::  - d) the relative magnitude of Sirius B
 
::  - e) the "color" (spectral class) of Sirius B
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
48. <!--AstroSizeWhitdwrfNeutstarQSO_5-->The course materials presented three arguments suggesting that a white dwarf is roughly the size of the earth.  Which best summarizes them?
 
::  - a) doppler-shift...period-of-pulsation...temperature-luminosity
 
::  + b) temperature-luminosity...redshift...quantum-theory-of-solids
 
::  - c) x-ray-emmission...doppler-shift...rotation-rate
 
::  - d) all of these are true
 
::  - e) HR-diagram-location...X-ray-emmision...spectral-lines
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
49. <!--AstroSizeWhitdwrfNeutstarQSO_6-->As of 2008, the percent uncertainty in the distance to the Crab nebula is approximately, 
 
::  - a) 0.1%
 
::  - b) 10%
 
::  - c) 100%
 
::  + d) 25%
 
::  - e) 1%
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
50. <!--AstroSizeWhitdwrfNeutstarQSO_7-->What was Messier doing when he independently rediscovered the Crab in 1758? 
 
::  - a) Attempting to count asteroids
 
::  - b) Looking for lobsters
 
::  - c) Attempting one of the first star charts
 
::  + d) Looking for a comet that he knew would be appearing in that part of the sky.
 
::  - e) Trying to measure the orbital radius of a planet
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
51. <!--AstroSizeWhitdwrfNeutstarQSO_8-->[[File:Gravitational red-shifting2.png|thumb|180px]]<br><br>What best explains this figure?
 
::  - a) The photon slows down as it goes uphill, and by c=f&lambda; it increases wavelength therefore by E=hf, it turns red.
 
::  - b) The photon slows down, by the Doppler shift, c=f&lambda;, and therefore by  E=hf it turns red.
 
::  - c) The photon loses energy, not speed.  By c=f&lambda; , it loses frequency, and by E=hf it increases wavelength and turns red.
 
::  - d) The photon slows down, by the Doppler shift, E=hf, and therefore by c=f&;lambda it turns red.
 
::  + e) The photon loses energy, not speed.  By E=hf, it loses frequency, and by c=f&lambda; it increases wavelength and turns red.
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
52. <!--AstroSizeWhitdwrfNeutstarQSO_9-->What causes the blue glow of the Crab nebula?
 
::  - a) the same emission found in a Lava lamp (ultra-violet)
 
::  - b) the curving motion of electrons in a magnetic field; such motion traps ultra-violet and blue light
 
::  + c) the curving motion of electrons in a magnetic field; such motion resembles a radio antenna
 
::  - d) the Doppler blue shift
 
::  - e) the Gravitational blue shift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
53. <!--AstroSizeWhitdwrfNeutstarQSO_10-->One way to determine the distance to a nebula or small cluster of clouds is to compare the angular expansion to the spectroscopic Doppler shift.  Two clusters (A and B) have the same spectroscopically measured velocity.  Cluster A is moving towards the observer and exhibits the greater angular expansion.  Which cluster is closer? 
 
::  - a) cluster B, because it exhibits less angular expansion
 
::  - b) either cluster might be more distant
 
::  + c) cluster A, because it exhibits greater angular expansion
 
::  - d) cluster B, because it exhibits a red Doppler shift
 
::  - e) cluster A, because it exhibits a blue Doppler shift
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
54. <!--AstroSizeWhitdwrfNeutstarQSO_11-->What causes the "finger-like" filamentary structure in the Crab nebula?
 
::  - a) cyclotron motion, causing the electrons to strike oxygen molecules
 
::  - b) electrons striking hydrogen molecules, like a lava lamp
 
::  + c) a light(low density) fluid underneath a heavy(high density) fluid, like a lava lamp
 
::  - d) electrons striking oxygen molecules, like a lava lamp
 
::  - e) a heavy (high density) fluid underneath a light (low density) fluid, like a lava lamp
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
55. <!--AstroSizeWhitdwrfNeutstarQSO_12--><math>KE=\frac{4\pi^2}{5}\frac{MR^2}{P^2}</math> is the kinetic energy of a solid rotating ball, where M is mass, R is radius, and P is period. And, <math>power=\frac{energy}{time}</math>.<br>You are banging espressos in a little coffeehouse with your astronomy friends, talking about a new SN remnant that closely resembles the Crab.  You have observed the pulsar, and wonder what the total power output of the nebula might be.  You know both the period of the pulsar, as well as <math>\tau</math>, which represents the amount of time you think the pulsar will continue pulsing if it continues slowing down at its present rate.  What formula do you write on your napkin?
 
::  + a) <math>power=\frac{4\pi^2}{5\tau}\frac{MR^2}{P^2}</math>
 
::  - b) <math>power=\frac{4\tau\pi^2}{5}\frac{MR^2}{P^2}</math>
 
::  - c) <math>power=\frac{5}{4\tau\pi^2}\frac{MR^2}{P^2}</math>
 
::  - d) <math>power=\frac{4\pi^2}{5\tau^2}\frac{MR^2}{P^2}</math>
 
::  - e) <math>power=\frac{4\pi^2}{5}\frac{MR^2}{P^2}\tau^4</math>
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
56. <!--AstroSizeWhitdwrfNeutstarQSO_13-->In one respect, the universie is arguably "young", considering how much complexity it contains.  This is often illustrated by a calculation of
 
::  - a) recalibration of supernovae luminosity
 
::  - b) cosmic expansion
 
::  - c) cosmic redshift
 
::  + d) chimps typing Shakespeare
 
::  - e) recalibration of supernovae relative magnitude
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
57. <!--AstroSizeWhitdwrfNeutstarQSO_14-->Comparing Hubble's original (1929) plot of redshift versus distance with the later one in 2007, the latter extends farther into space by a factor of
 
::  - a) 100
 
::  - b) 100,000
 
::  - c) 10,000
 
::  + d) 10
 
::  - e) 1000
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
58. <!--AstroSizeWhitdwrfNeutstarQSO_15-->The course materials present two cosmic expansion plots.   Hubble's original (1929) plot used
 
::  - a) Cepheid variables
 
::  - b) novae
 
::  + c) entire galaxies
 
::  - d) supernovae
 
::  - e) red giants
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
59. <!--AstroSizeWhitdwrfNeutstarQSO_16-->The course materials present two cosmic expansion plots.   The more recent (2007) plot used
 
::  - a) red giants
 
::  + b) supernovae
 
::  - c) Cepheid variables
 
::  - d) novae
 
::  - e) entire galaxies
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
60. <!--AstroSizeWhitdwrfNeutstarQSO_17-->Place yourself in an expanding raisinbread model of Hubble expansion.  A raisin originally situated at a distance of 4 cm expands out to 12 cm.  To what distance would a raisin originally situated at a distance of 2 cm expand?
 
::  - a) 2
 
::  + b) 6
 
::  - c) 8
 
::  - d) 3
 
::  - e) 4
 
</div>
 
 
<div style="page-break-inside:avoid;">
 
61. <!--AstroSizeWhitdwrfNeutstarQSO_18-->You at the center raisin of an expanding raisinbread model of Hubble expansion, and from your location a raisin originally situated at a distance of 1 cm expands out to a distance of 4 cm.  The nearest raisin with intelligent life is situated exactly halfway between your (central) location and the edge.  How would this second "intelligent" raisin view an expansion of a raisin 1 cm away?
 
::  - a) expansion from 1 cm to 2 cm (half of yours)
 
::  - b) expansion from 1 cm to 3 cm (since 3-1=2)
 
::  - c) expansion from 1 cm to 8 cm (twice yours).
 
::  - d) expansion from 1 cm to 9 cm (since 5-1=4)
 
::  + e) expansion from 1 cm to 4 cm (just like yours).
 
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62. <!--AstroSizeWhitdwrfNeutstarQSO_19-->Place yourself in an expanding raisinbread model of Hubble expansion.  A raisin originally situated at a distance of 2 cm expands out to 4 cm.  To what distance would a raisin originally situated at a distance of 4 cm expand?
 
::  + a) 8
 
::  - b) 6
 
::  - c) 2
 
::  - d) 3
 
::  - e) 4
 
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63. <!--AstroSizeWhitdwrfNeutstarQSO_20-->[[File:Light-clock.png|thumb]]This light clock is associated with 
 
::  - a) all of these are true
 
::  - b) doppler shift
 
::  - c) gravitational shift
 
::  - d) general relativity
 
::  + e) special relativity
 
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64. <!--AstroSizeWhitdwrfNeutstarQSO_21-->[[File:Light-clock.png|thumb]]Suppose the light clock involved a ball being tossed back and forth on a train going just under the speed of sound.  In contrast to the situation for light reflecting back and forth on a train going just under the speed of light, there is virtually no time dilation.  Why?
 
::  - a) Special relativity is valid only for objects travelling in a vacuum.
 
::  + b) The observer on the ground would perceive the ball to be travelling faster.
 
::  - c) The observer on the ground would perceive the width the train to be greater.
 
::  - d) The observer on the ground would perceive the ball to be travelling more slowly.
 
::  - e) The observer on the ground would perceive the width the train to be smaller.
 
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