
Originally Posted by
The Grand Puzzle
I began with two known masses which are travelling in parallel but opposing directions with a given distance between them which is perpendicular to their lines of motion. The difference in their velocities is also given and must be small enough so that the bodies will not escape each other and will instead produce closed, elliptical orbits. My initial observation was that the shape of the ellipses are identical for both bodies but that the dimensions are inversely proportional to the mass. I also noticed that a line drawn through the two bodies are only perpendicular to their lines of motion at their closest and furthest distances from each other and that the distance between these two points on the same orbit will describe the major axis of its ellipse.
Let's look at what is observed so far. Two bodies of masses M1 and M2 are orbitting each other and a line drawn between them will be perpendicular to their lines of motion at their closest and furthest distances from each other (Dc & Df). The sum of these two distances will equal the sum of the major axes of both orbits, so that 2(a1+a2)=Df+Dc, where (a) is the semi-major axis, equal to the distance from the center of the ellipse to its outermost point. The dimensions of each ellipse are inversely proportional to the mass of the body, so that the center of mass can be found at (1/M1)/(1/M1+1/M2)=(1/M1)/[(M1+M2)/M1M2]=M2/(M1+M2)=M2/MT of the distance from M1 to M2 or M1/MT from M2 to M1. If we are to use the center of mass as a frame of reference in order to stabilize the positions of the orbits around it, then the ratio of their individual velocities to the total difference in velocities at any given time will be directly related to the dimensions of each ellipse and must also be divided accordingly. If V is the difference in velocities at some point in their orbits, then V1=M2V/MT and V2=M1V/MT, so M1V1=M2V2.The semi-major axis of each ellipse is, of course, also proportional to its dimensions, so that we can find their lengths with a1=(Dc+Df)M2/2MT and a2=(Dc+Df)M1/2MT. Further observations show that Dc1Vc1=Df1Vf1=Vb1b1(MT/M2) and Dc2Vc2=Df2Vf2=Vb2b2(MT/M1), where Vc1 and Vf1 are the velocities for M1 at the closest and furthest distances and Vb1 is the velocity where the semi-minor axis (b1) crosses the ellipse on either side. One also finds that VcVf=Vb2 for each body, (Vb12/a1)+(Vb22/a2)=GMT/(a1+a2)2, and (Df/Dc)(Dc+Df)(Vf1+Vf2)2=2GMT (all quantities are positive).
The direction of the orbits will be perpendicular to their centers where it crosses the a and b axes. These orbits sweep out equal areas in equal times from the focus closest to where the orbits are closest (Dc), so that area per time is a constant. If we designate the distance from the center of the orbit to this focus as f, then the area swept out per time for Vc within an extremely small time interval is [(a-f)VcTi/2]/Ti=(a-f)Vc/2. For Vf it is (a+f)Vf/2. For Vb it is [(f+VbTi)b/2-fb/2]/Ti=Vbb/2. And for the entire orbit it is piab/Trev. These values are all equal, so (a-f)Vc/2=(a+f)Vf/2=Vbb/2=piab/T. Since a2-f2=b2, these terms can be recombined to show that (piab/T)2=(Vbb/2)2=[(a-f)Vc/2][(a+f)Vf/2]=(a2-f2)VcVf/4=b2VcVf/4, which becomes (2pia/T)2=Vb2=VcVf. Much can be determined by the formulas we have obtained so far. Further recombining yields formulas such as a/b=(Vb/2)(1/Vc+1/Vf) and GM23/MT2a1=(2pia1/T)2. This last formula demonstrates that Kepler's third law for the ratio of the cube of the semi-major axis to the square of the orbittal period requires some minor adjusting since it will only approach a constant for a body which is much more massive than the other (M2>>M1), but a discrepency will be noticed for bodies whose masses are close in value. (Is this last formula known? I have not found anything with these same simple results but much that says that there is a discrepency between Kepler's third law and the real orbits of planets. Perhaps I have corrected for this. Please let me know.)
If we know the initial conditions for M1, M2, Df, and Vo, where Vo is the original difference in velocities between the bodies in parallel lines of motion with a perpendicular distance between them of Df,we can now describe their orbits in detail relative to their center of mass. We will determine the values for M1, but the values for M2 can of course be found using the same equations by substituting M1 for M2 and M2 for M1. These values can be determined as follows:
Dc=Df2Vo2/(2GMT-DfVo2)
Vf1=VoM2/MT
a1=(Dc+Df)M2/2MT
Vc1=GM23/MT2a1Vf1
Vb1=(GM23/MT2a1)1/2
b1=Df1Vf1M2/MTVb1
f1=(a12-b12)1/2