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Wednesday, September 19, 2012

Astronomey

1.

 
What is spectroscopy?
  Student Response Value Correct Answer
the use of CCDs to capture light more efficiently than with photographic film  
a study of the geometry of rainbows  
a method to freeze atmospheric turbulence for better resolution  
Student Response an analysis of the way in which atoms absorb and emit light 100% Student Response  
an observational technique to measure the brightness of light at different colors  
Score: 1/1
 

2.

 
Which of these is the classic continuous spectrum?
  Student Response Value Correct Answer
sunlight  
a glowing nebula, such as M-42  
a fluorescent light  
Student Response a rainbow 100% Student Response  
a neon light  
Score: 1/1
 

3.

 
The three laws dealing with the creation of various spectra are due to:
  Student Response Value Correct Answer
Fraunhofer.  
Newton.  
Einstein.  
Student Response Kirchhoff. 100% Student Response  
Bohr.  
Score: 1/1
 

4.

 
A neon light (thin hot neon gas in a sealed tube) gives us:
  Student Response Value Correct Answer
Student Response a few bright emission lines, telling us the gas is neon. 100% Student Response  
nothing visible to us, but a hot of infrared lines as heat.  
a continuous spectrum, since the neon is hot enough to glow.  
a continuum, with dark lines identifying the neon atoms are present.  
a lot of random bright red lines due to the motion of the hot atoms.  
Score: 1/1
 

5.

 
In the atom, which particles gives the element its identify (atomic number)?
  Student Response Value Correct Answer
neutrons  
Student Response protons 100% Student Response  
electrons  
positrons  
neutrinos  
Score: 1/1
 

6.

 
The particles which enter into chemical reactions are the atom's:
  Student Response Value Correct Answer
neutrons.  
Student Response electrons. 100% Student Response  
mesons.  
positrons.  
protons.  
Score: 1/1
 

7.

 
An emission spectrum can be used to identify a(n)
  Student Response Value Correct Answer
neutron  
Student Response atom 100% Student Response  
electron.  
neutrino  
proton  
Score: 1/1
 

8.

 
The classical model of the hydrogen atom that explains its spectral line structure is due to:
  Student Response Value Correct Answer
Student Response Bohr. 100% Student Response  
Fraunhofer.  
Kirchhoff.  
Mendeleev.  
Newton.  
Score: 1/1
 

9.

 
In Bohr's model of the atom, electrons
  Student Response Value Correct Answer
Student Response only make transitions between orbitals of specific energies. 100% Student Response  
can be halfway between orbits.  
are spread uniformly through a large, positive mass..  
are not confined to specific orbits.  
move from orbit to orbit in many small steps.  
Score: 1/1
 

10.

 
The energy required to move an electron in a hydrogen atom from energy level 1 to energy level 2 is ( see section More precisely 4-1 section of the book)
  Student Response Value Correct Answer
12.1 eV  
10.2 eV Student Response  
13.1 eV  
12.75 eV  
Student Response 13.6 eV 0%  
Score: 0/1
 

11.

 
For hydrogen, the transition from the second to the fourth energy level produces
  Student Response Value Correct Answer
an ultraviolet absorption line.  
a red emission line.  
an infrared emission line.  
Student Response a blue green absorption line. 100% Student Response  
a violet emission line.  
Score: 1/1
 

12.

 
In a hydrogen atom, a transition from the third to the second energy level will produce
  Student Response Value Correct Answer
Student Response a red emission line. 100% Student Response  
an infrared emission line.  
a blue green absorption line.  
a violet emission line.  
an ultraviolet absorption line.  
Score: 1/1
 

13.

 
The observed spectral lines of a star are all shifted towards the red end of the spectrum.
Which statement is true?
  Student Response Value Correct Answer
The second law of Kirchhoff explains this.  
The star has a radial velocity towards us.  
Student Response This is an example of the Doppler effect. 100% Student Response  
This is an example of the photoelectric effect.  
The star is not rotating.  
Score: 1/1
 

14.

 
The broadening of spectral lines can be caused by:
  Student Response Value Correct Answer
thermal motion of the hot atoms.  
density of the hot medium.  
magnetic fields of the star.  
Student Response rotation of the star. 0%  
all of the above Student Response  
Score: 0/1
 

15.

 
Only a hot, thin gas can produce an emission line.
Student Response Value Correct Answer
False 0% True
Score: 0/1
 

16.

 
In the Bohr model, the transitions of electrons down to ground state produce the Lyman lines in the ultraviolet.
Student Response Value Correct Answer
True 100% True
Score: 1/1
 

17.

 
The shorter a wave's wavelength, the greater it's energy.
Student Response Value Correct Answer
True 100% True
Score: 1/1
 

18.

 
An X-ray photon has more energy than a visible photon.
Student Response Value Correct Answer
True 100% True
Score: 1/1
 

19.

 
All wavelengths of light travel at the same speed in a vacuum, and carry the same energy per photon.
Student Response Value Correct Answer
True 0% False
Score: 0/1
 

20.

 
Molecular spectra, like elemental ones, involve only the vibration of the particles.
Student Response Value Correct Answer
False 100% False
Score: 1/1
 

21.

 
Spectroscopy of a star can reveal its temperature, composition, and line-of-sight motion.
Student Response Value Correct Answer
True 100% True
Score: 1/1
 

22.

 
In our Sun, the spectral lines of hydrogen are weak, compared to their appearance in hotter stars.
Student Response Value Correct Answer
True 100% True
Score: 1/1

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