Page:Encyclopædia Britannica, Ninth Edition, v. 23.djvu/396

Rh No rela tive mo tion be tween satellite and planet when energy maxi mum or minimum Equa tions of mo mentum, energy, and no relative motion. Graphical illustra tion. and two imaginary, or all imaginary roots. The quartic may be derived from quite a different consideration, viz., by finding the con dition under which the satellite may move round the planet so that the planet shall always show the same face to the satellite, in fact, so that they move as parts of one rigid body. The condition is simply that the satellite's orbital angular velocity l=n, the planet's angular velocity of rotation, or y=l/x 3, since n=y and ri=O~J=a;. By substituting this value of y in the equation of momentum (104), we get as before x*-hx 3 + l = Q At present we have only obtained one result, viz., that, if with given moment of momentum it is possible to set the satellite and planet moving as a rigid body, it is possible to do so in two ways, and one of these ways requires a maximum amount of energy and the other a minimum; from this it is clear that one must be a rapid rotation with the satellite near the planet and the other a slow one with the satellite remote from the planet. In the three equations h = y + x (107), F=(A-a;) 2 -l/x 2 (108), aty=l (109), (107) is the equation of momentum, (108) that of energy, and (109) may be called the equation of rigidity, since it indicates that the two bodies move as though parts of one rigid body. To illustrate these equations geometrically, we may take as abscissa x, which is the moment of momentum of orbital motion, so that the axis of x may be called the axis of orbital momentum. Also, for equations (107) and (109) we may take as ordinate y, which is the moment of momentum of the planet's rotation, so that the axis of y may be called the axis of rotational momentum. For (108) we may take as ordinate Y, which is twice the energy of the system, so that the axis of Y may be called the axis of energy. Then, as it will be convenient to exhibit all three curves in the same figure, with a parallel axis of x, we must have the axis of energy identical with that of rotational momentum. It will not be necessary to consider the case where the resultant moment of momentum h is negative, because this would only be equivalent to i-eversing all the rotations; h is therefore to be taken as essentially positive. Then the line of momentum whose equation is (107) is a straight line inclined at 45 to either axis, having positive intercepts on both axes. The curve of rigidity whose equation is (109) is clearly of the same nature as a rectangular hyperbola, but it has a much more rapid rate of approach to the axis of orbital momentum than to that of rotational momentum. The intersections (if any) of the curve of rigidity with the line of momentum have abscissae which are the two roots of the quartic x 4 - hx 3 +l = 0. The quartic has, therefore, two real roots or all imaginary roots. Then, since x=/r, the intersection which is more remote from the origin indicates a configuration where the satellite is remote from the planet; the other gives the configuration where the satellite is closer to the planet. We have already learnt that these two cor respond respectively to minimum and maximum energy. When x is very large, the equation to the curve of energy is Y= (h - a;) 2, which is the equation to a parabola with a vertical axis parallel to Y and distant h from the origin, so that the axis of the para bola passes through the intersection of the line of momentum with the axis of orbital momentum. When x is very small, the equation becomes Y= - 1/z 2. Hence the axis of Y is asymptotic on both sides to the curve of energy. Then, if the line of mo mentum intersects the curve of rigidity, the curve of energy has a maximum vertically underneath the point of intersection nearer the origin and a minimum underneath the point more remote. But, if there are no intersections, it has no maximum or minimum. Fig. 9 shows these curves when drawn to scale for the case of the earth and moon, that is to say, with h =4. The points a and b, which are the maximum and minimum of the curve of energy, are supposed to be on the same ordinates as A and B, the intersections of the curve of rigidity with the line of momentum. The in tersection of the line of momentum with the axis of orbital momentum is denoted by D, but in a figure of this size it necesFig. 9. sarily remains indistinguishable from B. As the zero of energy is quite arbitrary, the origin for the energy curve is displaced down wards, and this prevents the two curves from crossing one another in a confusing manner. On account of the limitation imposed we neglect the case where the quartic has no real roots. Every point of the line of momentum gives by its abscissa and ordinate the square root of the satellite's distance and the rotation of the planet, and the ordinate of the energy curve gives the energy corresponding to each distance of the satellite. Part of the figure has no physical meaning, for it is impossible for the satellite to move round tho planet at a distance less than the sum of the radii of the planet and satellite. For example, the moon's diameter being about 2200 rniles, and the earth's about 8000, the moon's distance cannot be less than 5100 miles. Accordingly a strip is marked off and shaded on each side of the vertical axis within which the figure has no physical meaning. The point P indicates the present configura tion of the earth and moon. The curve of rigidity x 3 y="i is the same for all values of h, and by moving the line of momentum parallel to itself nearer to or further from the origin, we may represent all possible moments of momentum of the whole system. The smallest amount of moment of momentum with which it is Least mopossible to set the system moving as a rigid body, with centrifugal mentum force enough to balance the mutual attraction, is when the line of for which momentum touches the curve of rigidity. The condition for this no relais clearly that the equation x 4 - hx 3 + 1 = should have equal roots, tive moIf it has equal roots, each root must be f A, and therefore tion pos8ible whence & 4 =4 4 /3 3 or 7i=4/3 J =175. The actual value of h for the moon and earth is about 4; hence, if the moon-earth system were started with less than % of its actual moment of momentum, it would not be possible for the two bodies to move so that the earth Maxishould always show the same face to the moon. Again, if we travel mum along the line of momentum, there must be some point for which number yx 3 is a maximum, and since yx 3 =n/ft there must be some point of days in for which the number of planetary rotations is greatest during one month. revolution of the satellite; or, shortly, there must be some con figuration for which there is a maximum number of days in the month. Now yx 3 is equal to x 3 (h-x), and this is a maximum when a; =|A and the maximum number of days in the month is ($h) 3 (h- |/i) or 3 3 /i. 4 /4 4; if A is equal to 4, as is nearly the case for the earth and moon, this becomes 27. Hence it follows that we now have very nearly the maximum number of days in the month. A more accurate investigation in a paper on the "Precession of a Viscous Spheroid" in Phil. Trans., part i., 1879, showed that, taking account of solar tidal friction and of the obliquity to the ecliptic, the maximum number of days is about 29, and that we have already passed through the phase of maximum. We will now consider the Discusphysical meaning of the figure. It is assumed that the resultant sion of moment of momentum of the whole system corresponds to a positive figure. rotation. Now imagine two points with the same abscissa, one on the momentum line and the other on the energy curve, and suppose the one on the energy curve to guide that on the momentum line. Then, since we are supposing frictional tides to be raised on the planet, the energy must degrade, and however the two points are set initially the point on the energy curve must always slide down a slope, carrying with it the other point. Looking at the figure, we see that there are four slopes in the energy curve, two running down to the planet and two down to the minimum. There are therefore four ways in which the system may degrade, according to the way it was started; but we shall only consider one, that corresponding to the portion AB&a of the figure. For the part of the line of momentum AB the month is longer than the day, and this is the case with all known satellites except the nearer one of History of Mars. Now, if a satellite be placed in the condition A that is to satellite say, moving rapidly round a planet which always shows the same as energy face to the satellite the condition is clearly dynamically unstable, degrades. for the least disturbance will determine whether the system shall degrade down the slopes ac or ab that is to say, whether it falls into or recedes from the planet. If the equilibrium breaks down by the satellite receding, the recession will go on until the system has reached the state corresponding to B. It is clear that, if the intersection of the edge of the shaded strip with the line of mo mentum be identical with the point A, which indicates that the satellite is just touching the planet, then the two bodies are in effect parts of a single body in an unstable configuration. If, therefore, the moon was originally part of the earth, we should expect to find this identity. Now in fig. 9, drawn to scale to re present the earth and moon, there is so close an approach between the edge of the shaded band and the intersection of the line of momentum and curve of rigidity that it would be scarcely possible to distinguish them. Hence, there seems a probability that the two bodies once formed parts of a single one, which broke up in consequence of some kind of instability. This view is confirmed by the more detailed consideration of the case in the paper on the "Precession of a Viscous Spheroid," already referred to, and sub sequent papers, in the Philosophical Transactions of the Royal Society. 1 1 For further consideration of this subject see a series of papers by Mr G. H. Darwin, in Proceed, and Trans, of the Royal Society from 1878 to 1881, and Appendix Q (b) to part ii. vol. i. of Thomson and Tait's Nat. Phil., 1883.