The main results of a study of a catalogue of physical parameters of 1041 spectroscopic binaries are presented. The distribution of spectroscopic binaries over all main parametersM1, a, e, M1/M2, P, and certain dependencies between some of them have been found. (1) It appears that among bright (mv≲3m–5m) stars withM≳1M⊙, about 40% are apparently spectroscopic binaries with comparable masses of components. (2) The majority of spectroscopic binaries with the ratio of the large semiaxis of the orbit to the radius of the primarya/R1≲20, have eccentricities close to zero. This is probably a consequence of the tidal circularization of orbits of close binaries by viscous friction. (3) The discovery of duplicity of double-line spectroscopic binaries is possible only if the semiamplitude of radial velocityK1 is almost 10 times higher than the semiamplitude of the radial velocity of a single-line spectroscopic binary of the same mass. (4) Double-line spectroscopic binaries witha/R⊙≲6(M1/M⊙)1/3,M1≈M2≳1.5M⊙ are almost almost absent, and the number of stars witha/R⊙≲6(M1/M⊙)1/3,M1≈1.5M⊙ is relatively low. (5) The distribution of unevolved SB stars over the large semiaxis may be described by the expression d(Nd/Nt)≈0.2 d loga for 6(M1/M⊙)1/3≲a/R⊙≲100. (6) The intial mass-function for primaries of spectroscopic binaries is the same Salpeter function dNd≈M1−2.35dM1 for 1≲M1/M⊙≲30. (7) It is possible to explain the observed ratio of the number of single-line spectroscopic binaries to the number of double-line binaries if one assumes that the average initial mass ratio is close to 1 and that the mass of the postmass-exchange remnant of the primary exceeds the theoretical one and/or that half of the angular momentum of the system is lost during mass-exchange. (8) The above-mentioned distributions ofM1 anda and assumptions on the mass of remnant and/or momentum loss also allow us to explain the observed shapes of dN/dM, dN/dq, and dN/da distributions after some selection effects are taken into account.