COS 126

N-Body Simulation
Programming Assignment

In 1687 Sir Isaac Newton formulated the principles governing the the motion of two particles under the influence of their mutual gravitational attraction in his famous Principia. However, Newton was unable to solve the problem for three particles. Indeed, in general, systems of three or more particles can only be solved numerically. Write a program to simulate the motion of N particles, mutually affected by gravitational forces, and animate the results. Such methods are widely used in cosmology, semiconductors, and fluid dynamics to study complex physical systems. Scientists also apply the same techniques to other pairwise interactions including Coulombic, Biot-Savart, and van der Waals.

The physics. We review the equations governing the motion of the particles according to Newton's laws of motion and gravitation. Don't worry if your physics is a bit rusty; all of the necessary formulas are included below. We'll assume for now that the position (rx, ry) and velocity (vx, vy) of each particle is known. In order to model the dynamics of the system, we must know the net force exerted on each particle.

The numerics.  We use the leapfrog finite difference approximation scheme to numerically integrate the above equations: this is the basis for most astrophysical simulations of gravitational systems. In the leapfrog scheme, we discretize time, and update the time variable t in increments of the time quantum Δt. We maintain the position (rx, ry) and velocity (vx, vy) of each particle at each time step. The steps below illustrate how to evolve the positions and velocities of the particles.

  1. For each particle: Calculate the net force (Fx, Fy) at the current time t acting on that particle using Newton's law of gravitation and the principle of superposition.

  2. For each particle:

    1. Calculate its acceleration (ax, ay) at time t using the net force computed in Step 1 and Newton's second law of motion: ax = Fx / m, ay = Fy / m.

    2. Calculate its new velocity (vx, vy) at the next time step by using the acceleration computed in Step 2a and the velocity from the old time step: Assuming the acceleration remains constant in this interval, the new velocity is (vx + Δt ax, vy + Δt ay).

    3. Calculate its new position (rx, ry) at time t + Δt by using the velocity computed in Step 2b and its old position at time t: Assuming the velocity remains constant in this interval, the new position is (rx + Δt vx, ry + Δt vy).

  3. For each particle: Draw it using the position computed in Step 2.
The simulation is more accurate when Δt is very small, but this comes at the price of more computation. Use Δt = 25,000 in this assignment for a reasonable tradeoff.

Creating an animation. Draw each particle at its current position using standard draw, and repeat this process at each time step. By displaying this sequence of snapshots (or frames) in rapid succession, you will create the illusion of movement. After each time step (i) draw the background image starmap.jpg, (ii) redraw all the bodies in their new positions, and (iii) control the animation speed using

Input format. The input file is a text file that contains the information for a particular universe. The first value is an integer N which represents the number of particles. The second value is a real number R which represents the radius of the universe: assume all particles will have x- and y-coordinates that remain between -R and R. Finally, there are N rows, and each row contains 6 values. The first two values are the x- and y-coordinates of the initial position; the second two values are the x- and y-coordinates of the initial velocity; the third value is the mass; the last value is a String that is the name of an image file used to display the particle. As an example, the input file planets.txt contains data for our solar system (in SI units).

% more planets.txt
1.496e11 0.000e00 0.000e00 2.980e04 5.974e24 earth.gif
2.279e11 0.000e00 0.000e00 2.410e04 6.419e23 mars.gif
5.790e10 0.000e00 0.000e00 4.790e04 3.302e23 mercury.gif
0.000e00 0.000e00 0.000e00 0.000e00 1.989e30 sun.gif
1.082e11 0.000e00 0.000e00 3.500e04 4.869e24 venus.gif
The subdirectory nbody from the COS 126 ftp site contains the planets.txt file, images of the planets, and many other sample universes.

Your program.   Write a program that reads in the universe from standard input using StdIn, simulates its dynamics using the leapfrog scheme described above, and animates it using StdDraw. Maintain several arrays to store the data. To make the computer simulation, write an infinite loop that repeatedly updates the position and velocity of the particles. When plotting, use StdDraw.setXscale(-R, +R) and StdDraw.setYscale(-R, +R) to scale the physics coordinates to the screen coordinates.

Finishing touch. For a finishing touch, play the theme to 2001: A Space Odyssey using StdAudio and the file 2001.mid. It's a one-liner using the method

Compiling and executing your program. Follow these instructions [ Windows · Mac · Linux ] to configure the command-line on your system. To compile your program from the command line, type:

% javac

in your Terminal application. To execute your program from the command line, redirecting from the file planets.txt to standard input, type:

% java NBody < planets.txt

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Submission. Submit Also submit a readme.txt file and answer the questions.

Extra credit. Submit a universe (in our input format) along with the necessary image files. If its behavior is sufficiently interesting, we'll award extra credit.

Challenge for the bored. There are limitless opportunities for additional excitement and discovery here. Try adding other features, such as supporting elastic or inelastic collisions. Or, make the simulation three-dimensional by doing calculations for x-, y-, and z-coordinates, then using the z coordinate to vary the sizes of the planets. Add a rocket ship that launches from one planet and has to land on another. Allow the rocket ship to exert force with consumption of fuel.

Copyright © Robert Sedgewick and Kevin Wayne.