By M. M. Woolfson

ISBN-10: 0198504233

ISBN-13: 9780198504238

ISBN-10: 019850425X

ISBN-13: 9780198504252

ISBN-10: 0585484279

ISBN-13: 9780585484273

Computing device simulation is more and more utilized in physics and engineering to foretell the possible consequence of experiments and to help of their interpretation. this article for undergraduates illustrates the elemental options with various easy courses and difficulties drawn from quite a lot of disciplines.

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**Extra info for An introduction to computer simulation**

**Sample text**

For calculations involving the solar system it is convenient to use solar system units, where unit mass is the mass of the Sun, unit distance is the astronomical unit (AU) and unit time is one year. For such a system the gravitational constant, G, is 4n2. 3. The program TROJANS can be run with any specified body as origin. 3 are used with the sun specified as origin then the asteroids stay rigidly in their original positions. However, with some modification of the parameters from their ideal values the asteroids do not stay in their initial positions but oscillate about them - which illustrates the stability of their equilibrium positions.

However, many problems of physical interest are not steady-state, so that time is introduced as another independent variable, and/or may be in more than one dimension, which also increases the number of independent variables. Such problems are often expressed in the form of partial differential equations and we shall now see how to generalize the finite-difference concept into these areas by application to the simple diffusion equation. 3 The diffusion equation In Fig. 4 we show a section of a column of solution, of uniform unit crosssection, with a varying concentration along its length.

Since the satellite will not be perfectly elastic there will be hysteresis effects and some of the mechanical energy will be converted into heat which is radiated away. The overall effect is that while the system as a whole is losing mechanical energy it must conserve Models and simulation Fig. 2); (b) an enlarged view of the motion of the leading asteroid. angular momentum. For a planet of mass M and a satellite of mass m («M), in an orbit of semi-major axis a and eccentricity e, the total energy is and the angular momentum is If E is to decrease then a must become smaller, but if H is then to be constant then e must become smaller - that is to say, that the orbit must round off.

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