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Using our photometric observations taken between 1996 and 2013 and otherpublished data, we derived properties of the binary near-Earth asteroid(175706) 1996 FG3 including new measurements constraining evolution of themutual orbit with potential consequences for the entire binary asteroidpopulation. We also refined previously determined values of parameters of bothcomponents, making 1996 FG3 one of the most well understood binary asteroidsystems. We determined the orbital vector with a substantially greater accuracythan before and we also placed constraints on a stability of the orbit.Specifically, the ecliptic longitude and latitude of the orbital pole are266{\deg} and -83{\deg}, respectively, with the mean radius of the uncertaintyarea of 4{\deg}, and the orbital period is 16.1508 +/- 0.0002 h (all quoteduncertainties correspond to 3sigma). We looked for a quadratic drift of themean anomaly of the satellite and obtained a value of 0.04 +/- 0.20 deg/yr^2,i.e., consistent with zero. The drift is substantially lower than predicted bythe pure binary YORP (BYORP) theory of McMahon and Scheeres (McMahon, J.,Scheeres, D. [2010]. Icarus 209, 494-509) and it is consistent with the theoryof an equilibrium between BYORP and tidal torques for synchronous binaryasteroids as proposed by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D.[2011]. ApJ Letters, 736, L19). Based on the assumption of equilibrium, wederived a ratio of the quality factor and tidal Love number of Q/k = 2.4 x 10^5uncertain by a factor of five. We also derived a product of the rigidity andquality factor of mu Q = 1.3 x 10^7 Pa using the theory that assumes an elasticresponse of the asteroid material to the tidal forces. This very low valueindicates that the primary of 1996 FG3 is a 'rubble pile', and it also callsfor a re-thinking of the tidal energy dissipation in close asteroid binarysystems.

The binary near-Earth asteroid (175706) 1996 FG3 - An observational constraint on its orbital evolution