References

  • Roy, A.E. Orbital Motion: 3rd edition. 1988. Adam Hilger: Philadelphia
  • Dave Arnold: College of the Redwoods
  • Feynman, Richard, Robert Leighton, and Matthew Sands.  The Feynman Lectures on Physics,

    •     Vol. 1. 1963. Addison-Wesley: Reading, Massachusetts
    Simmons, George F. Differential Equations with Applications and Historical Notes.
        1972. McGraw-Hill
     
     
     
     
     

    Matlab m-files

  • pscript3.m
  • planet2.m
  • r.m

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        The file pscript3.m is a function file which calls both planet2.m and r.m.  The input for pscript3 is, in this order:
     

  • The amount of time you want the solver to run for (2p is usually sufficient).
  • A four entry row vector with the initial x-position, x-velocity, y-position, and y-velocity of the orbiting mass.
  • The mass of the larger object (use large numbers, like 1e12)
  • The mass of the smaller object (use large numbers, but not as large as the larger object)
  • An optional initial two entry row vector with the intial x and y velocity of the central object.  This entry is not necessary if a stationary central body is desired.

    •  

     

        There are default settings for the program so that if you just type "pscript3" at the matlab prompt, you will get a result.

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