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mg   r 
                                                                                                              (6.45)
                                                             L
                   take into account that    IL         

                                                         mg      r
                                                                 .                                             (6.46)
                                                              I  
                  Thereby  we deduced  formula of angular velocity  of precession
                           Gyroscopic precession also plays a large role in the flight controls
                  on  helicopters.  Since  the  driving  force  behind  helicopters  is  the  rotor

                  disk (which rotates), gyroscopic precession comes into play. If the rotor
                  disk  tilted forward (to gain forward velocity), its rotation requires that
                  the  downward  net  force  on  the  blade  be  applied  roughly  90  degrees

                  (depending on blade configuration) before, or when the blade is to one
                                                                        side  of  the  pilot  and  rotating
                                                                        forward.
                                                                                In  astronomy,  precession

                                                                        refers  to  any  of  several
                                                                        gravity-induced,  slow  and
                                                                        continuous  changes  in  an

                                                                        astronomical body's rotational
                                                                        axis or orbital path. Precession
                                                                        of  the  equinoxes,  perihelion

                                                                        precession, and changes in the
                                                                        tilt  of  the  Earth's  axis  to  its
                                                                        orbit,  and  the  eccentricity  of

                                                                        its  orbit  over  tens    thousands
                                                                        years are all important parts of
                            Figure 6.20                                 the  astronomical  theory  of
                                                                        ages.  Earth  goes  through  one

                                                                        such  complete  precessional
                  cycle in a period of approximately 26,000 years or 1° every 72 years,
                  during which the positions of stars will slowly change in both equatorial

                  coordinates  and  ecliptic  longitude.  Over  this  cycle,  Earth's  north axial
                  pole moves from where it is now, within 1° of Polaris, in a circle around
                  the ecliptic pole, with an angular radius of about 23.5 degrees.









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