Motion of particles close to the Earth

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SUMMARY

The discussion focuses on the motion of particles close to Earth, analyzed through two approaches: Lagrangian mechanics and a rotating reference frame. The equations of motion derived from Lagrangian mechanics are given by d/dt(dx/dt) = -G*M_earth*x/((x^2+y^2+z^2)^3/2) and similar for y and z. The rotating reference frame equations include terms for Coriolis and centrifugal forces. The participant expresses uncertainty about the completeness of the Lagrangian approach and the complexity of the rotating frame solution, emphasizing the need for numerical methods and conservation laws for accurate analysis.

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  • Lagrangian mechanics
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  • Newtonian mechanics
  • Numerical methods for solving differential equations
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Physicists, aerospace engineers, and students studying mechanics who are interested in the dynamics of particles in gravitational fields and the application of Lagrangian and numerical methods in solving motion problems.

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Homework Statement
Problem: A spherical body is rotating with angular velocity (=Omega constant) on the z-axis. A person throws 3 balls with initial speeds v0:
1-) First ball to the north with angle pi/4 to the surface
2-) Second ball pi/2 degrees to the surface (right upwards)
3-) Third ball to the south with angle pi/4 to the surface

Find where the balls will land. Assume v<v_escape at any time.
Relevant Equations
v<v_escape at any time;
Radius of the planetary body = a;
Initial latitude = theta_0
I tried to solve the problem in 2 ways, first using lagrangian mechanics and second by putting a rotating reference frame on the initial take-off point.

However I cannot be sure if the equations of motion for the two solutions came out the same.

A-) Equations of motion from Lagrangian Solution:

d/dt(dx/dt) = -G*M_earth*x/((x^2+y^2+z^2)^3/2);
d/dt(dy/dt) = -G*M_earth*y/((x^2+y^2^z^2)^3/2),
d/dt(dz/dt) = -G*M_earth*z/((x^2+y^2+z^2)^3/2);

B-) Equations of motion from the rotating reference frame solution:
d/dt(dx/dt) = 2*omega*(dy/dt*cos(theta)-dz/dt*sin/theta);
d/dt(dy/dt) = -2*omega*dx/dt*cos(theta) - omega^2*a*sin(theta)^2-g;

When I use the equations from Lagrangian, I feel like I omitted something leaving some terms relating the orbital motion out. I am not sure if any of the two solutions are true. After I find the equations of motion, I will use the equations and the initial conditions to numerically solve the problem. Then I will use conservation laws at the problem to choose the best numerical method to solve this problem. However I am stuck at this stage. I would be glad if anyone helped.

coriolis.JPG
 
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v<v_escape makes sure it lands again, but there are useful approximations that only work if v<<v_escape. Without these things get complicated.

Solving this analytically in the rotating reference frame will be really messy or even impossible.

The equations of motion in your first approach are simply from Newtonian mechanics. They work, of course. In practice you probably want to use the knowledge that free-fall trajectories are ellipses, and calculate parameters of these ellipses.
 

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