•Possible to determine mass of a binary system
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•Find ρ = 2 g/cm3, consistent with its recent spectral classification as an S-type asteroid
•Knowing orbital period and radius allows one to determine the total mass of the system from Kepler’s Third Law
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•Assuming both asteroids have the same density and are roughly spherical, we can then find an expression for the density
 density
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This value is likely to be very close to the actual density, as the primary’s rotation rate is very near to the break up velocity.  This implies that the primary cannot be far from edge-on, or else the true rotation rate would be too fast.  If we assume that the secondary lies in the same plane as that of the primary’s rotation, then the orbit would be approximately edge-on too.  We estimate that the primary can be no more that 30 from edge-on, at which point the correction factor sin i becomes less than 15%.

These asteroids are composed of the various silicate mixtures having mineral densities of approximately 3 g/cm3 (not taking into account porosity).