1. What makes astrometric wobbles easier to observe?

a. If the star is further away from the Sun.
b. If the largest companion is more massive.
c. If the largest companion is closer to the star.
d. All of the above.
e. None of the above.

2. Which of the following is most likely to be detected orbiting a star like the Sun using the radial velocity method?

a. A brown dwarf orbiting at 75 AU.
b. A terrestrial world orbiting at 0.1 AU.
c. A terrestrial world orbiting at 2 AU.
d. A jovian world orbiting at 0.2 AU.
e. None of the above.

3. What can we say about the inclination of a transiting system?

a. We are observing the system pole-on (i.e. viewing from directly above or below the plane).
b. We are observing edge-on (i.e. from within the plane).
c. The orbiting planet must be close to the central star.
d. The orbiting planet must be far from the star.
e. None of the above.

4. Which of the following would be the easiest to detect around an M dwarf with direct imaging?

a. A brown dwarf orbiting at 150 AU.
b. A brown dwarf orbiting at 50 AU.
c. A jovian world orbiting at 10 AU.
d. A terrestrial world orbiting at 1 AU.
e. None of the above.

5. Why would we expect brown dwarfs to have more molecules in their spectra than hotter stars?

a. Molecules are broken into atoms in hot stars.
b. Brown dwarfs have less H and He, leaving more C, N, and O to form molecules.
c. The lower mass of brown dwarfs can't hold down atoms, so they escape, leaving the molecules.
d. All of the above contribute.
e. None of the above.

Home

Last modified 29 April, 2007. © Gregory C. Sloan.