Lab 8: The Doppler Effect---The Rotation of Mercury


Sections

  1. Student Preparation which includes Quiz Preparation.
  2. Special Instructions for Instructors
  3. Startup Presentation
  4. Background Notes They may be incomplete or not exist.
  5. Deep Background Notes Intended primarily for instructors, but students can benefit from them too. They may be incomplete or not exist.


  1. Student Preparation

  2. Required Preparation for Section 9, but it is suggested for all sections plus whatever your section instructor requires.

    Lab Preparation:

    1. Read Lab 8
    2. Read a sufficient amount of the articles linked to the following terms etc. so that you can define and/or understand the terms etc. at the level of our class: Doppler effect, electromagnetic spectrum, Mercury, Mercury's spin-orbit resonance, radar, radial velocity.
    3. Write out the definitions required in Part A of Lab 8.

    Suggested Supplementary Preparation. The items are often alternatives to the required preparation.

    1. Bennett (2008 edition): p. 149--157 and 163--174 on light and p. 215 on Mercury's spin-orbit resonance, or the corresponding pages in similar books.
    2. IAL 12: The Moon and Mercury: Spin-Orbit Resonance.
    3. Background Notes

    Quiz Preparation:


  3. Special Instructions for Instructors

    1. Check as needed:
      1. Usual Startup
      2. Usual Shutdown
    2. This is an indoor lab. So you do NOT have to check the weather at NWS 7-day forecast, Las Vegas, NV in advance and by personal visual inspection at/during the lab period.

    3. You do NOT set up the C8 telescopes on the roof before the lab period and review their usage well in advance if needed.

    4. Objectives: This lab illustrates how the Doppler effect, which applies to all wave phenomena, can be used with electromagnetic radiation (EMR) to determine the motion of astro-bodies. We use radar astronomy to determine the rotation period and orbital velocity of Mercury. It is NOT a high accuracy lab.

      The students will learn a little about electromagnetic radiation (EMR), frequency, the Doppler effect, and radar astronomy. The geometry in the lab may be a bit more than they can absorb in the lab period.

    5. If you can or are ordered to, you will use a projector to illustrate CLEA rotation of Mercury lab.


  4. Startup Presentation

  5. The Startup Presentation should usually be no more than about 10 minutes. Students lose patience and want to get at the work---and that is right---labs are active learning, not passive learning.

    For this lab a few bullets in point form written on the board with drawn diagrams and handwaving might be best.

    You will have to give up presenting when you run out of time (10 minutes or so)---and leave the rest of the things you could say to TA mode.

    1. First all groups go the computers and launch open the lab 8 folder and launch the CLEA rotation of Mercury lab.

    2. You will need to fill in the date and time: us 2012 Nov05, 8 pm.

      The other settings are computed for you.

      Then lauch a radar pulse to Mercury.

      It will take 13 minutes---real-time minutes---to get back.

      So now I will give a presentation which will die in 10 minutes or so no matter where it gets too.

    3. Electromagnetic radiation (EMR) is the generalization of light to all invisible-to-the-human-eye forms: you are familiar with many of these: high frequency to low frequency: gamma rays, X-rays, ultraviolet, visible light, infrared, microwave, radio, etc.

    4. The full range of EMR is called the electromagnetic spectrum.

    5. Frequency, or alternatively wavelength, charaterizes EMR.

    6. Simply put frequency is the number of wave cycles that go past some point per unit time.

    7. The standard unit is the inverse second: 1 s**(-1)=1 hertz=1 Hz.

    8. kHz (10**3 Hz), MHz (10**6 Hz), GHz (10**9 Hz) are the more common units for radio waves such as we use in the lab.

    9. Say you are at rest in some inertial frame of reference and measure a particular frequency for an EMR beam passing by.

    10. Then you plow into the EMR beam head-on.

    11. The wave cycles hit you more frequently. The faster you plow in, the more frequently they hit you. Their frequency has been increased by your motion.

    12. Now you run away right away from the EMR beam.

    13. The wave cycles hit you less frequently. The faster you run away, the less frequenctly they hit you. Their frequency has been decreased by your motion.

      In the limiting case, that you run away at the vacuum light speed c the frequency will go to zero. You can't reach c, of course, but nothing forbids you from coming arbitrarily close, in principle.

    14. This change in frequency of EMR with the observer motion along the beam direction is the Doppler effect.

    15. The "observer" could be a source or a receiver.

    16. There is a Doppler effect for motion perpendicular to the beam direction called the transverse Doppler effect, but it is usually much too small to detect---and we won't worry about it.

    17. The approximate Doppler effect we will use in this lab is:

                   df/f=v/c , 
      
                   where df is the change frequency,
      
                   f is the initial or final frequency 
                     (it doesn't matter which to our level of error),
       
                   v is the velocity of the "observer" along the beam direction relative to whatever the
                     initial frame of rest was.
      
                   v>0 for an "observer" plowing into the waves
      
                   v<0 for an "observer" running away from the waves. 
      
                   This formula is only valid for df/f<<1, and that is why
                   can be either the initial or final frequency.
      
                   If df>0, the frequency shift is
                            called a blueshift.
      
                   If df<0, the frequency shift is 
                            called a redshift.
      
             

      A derivation of this formula is given in the Background Notes: Doppler Effect.

      But you-all don't need to know that---but it would be good for your soul.

    18. In this lab, we bounce a radar pulse off Mercury with the CLEA rotation of Mercury lab.

    19. We neglect the Earth's motion and other complicating effects.

    20. What happens to the radar pulse frequency?

      Well Mercury "observes" the radar pulse with frequency shift given by

      
                   df_1/f=v/c , where v is Mercury's
                              velocity in the direction of the Earth
                              or as we call the 
                              radial velocity
                              of Mercury
                              from the Earth's
                              perspective.
      
                   So Mercury observes
                   frequency
      
                   f+df_1
      
                   and reflects some signal back to Earth.
      
                   Now Earth
                   is plowing into the return signal at velocity v relative to 
                   Mercury, and so
                   there is another shift given by
      
                   df_2/(f+df)= approximately df_2/f=v/c   .
      
                   The frequency 
                   measured at Earth is thus
       
                   f+df_1+df_2 .
      
                   The total shift is just 
      
                   df=df_1+df_2 and is given by
      
                   df/f=2v/c .
      
                   So that is where the mysterious 2 comes from in this lab.
      
                   If Mercury is moving
                   toward Earth, v>0 and df>0.
      
                   Otherwise, v<0 and df<0.
              

    21. Now Mercury is actually an extended rotating object.

      We assume for simplicity that its rotation axis is perpendicular to the Mercury-Earth line.

      Because it is an extended rotating object, there is not one signal with one shifted frequency coming back from Mercury, but a continuum range of signals with a continuum range of shifted frequencies.

      And this range varies with time since different parts of Mercury are different distances away---so we get a time range of returning signals.

      The returning first signal that comes back comes from sub-radar point---the surface point of Mercury directly on the Mercury-Earth line.

      This reflection region expands into an annulus that grows from the sub-radar point until it reaches Mercury's limb (the circumference region of Mercury as seen on the sky).

      After the limb signal returns, the radar pulse cannot reflect anymore and the returning signals die off abruptly.

    22. At any time, the returning signal has a range of a continuum range of shifted frequencies that extends from

                  df_r/f=v_r/c  , where v_r=v-v_rot*sin(theta)
                  
                  to
      
                  df_b/f=v_b/c  , where v_b=v+v_rot*sin(theta)
      
                  where r stands for reddest and b for bluest,
      
                  theta is the angle of the annulus reflection region from the sub-radar point
                  with the angle subtended at Mercury's center,
      
                  and v_rot is Mercury's
                  equatorial rotation velocity.
             

      Do NOT worry about the derivation of this formula.

      We can solve for v_rot:

                 v_rot=(v_b-v_r)/[2*sin(theta)]=(c/f)*(df_b-df_r)/[2*sin(theta)]  ,
      
                      which is undefined as theta goes to zero, but it doesn't go 
                      to infinity formally since df_b-df_r goes to zero likewise
                      as theta goes to zero.
      
                      Actual observed spectra have noise and are averages over 
                      some range of time.
                      So one does not see a sharp spike in 
                      frequency
                      as theta goes to zero, but a sort of broadened peak for which
                      df_b and df_r not really definable.
             

      You feed in df_r and df_b into the appropriate fields in the Excel spreadsheet and the other required data, and the Excel spreadsheet will calculate Mercury's rotation period P:

                P=2*pi*R_Mercury/v_rot  , where R_Mercury is 
      
                        Mercury's radius.
             

      This rotation period is relative to the fixed stars which define an inertial frame.

      So it is a sidereal time interval and NOT the Mercurian solar day P_sol which is actually twice the Merurian orbital period.

      Mercury's rotation period P and orbital period P_orb are locked in a Mercury's 3:2 spin-orbit resonance: P_orb:P=3:2.

      Gravitational effects have driven Mercury to this Mercury's 3:2 spin-orbit resonance and drive it back toward it if perturbed off the exact 3:2 ratio.

      So we actually have the ratio P_sol:P_orb:P=4:3:2.

    23. How do you identify df_r and df_b from the somewhat noisy returning signal spectrum?

      Where the signal spectrum seems to dive steeply at the red and blue ends before it disappears into background noise.

    24. The rest of the lab and questions, we will learn about as we go along.


  6. Background Notes: The Doppler Effect---The Rotation of Mercury


  7. Deep Background Notes: The Doppler Effect---The Rotation of Mercury

    1. Waves
    2. Electromagnetic Radiation
    3. Doppler Effect
    4. Relativisitic Doppler Effect
    5. Sound Doppler Effect