We present an analysis of our observations of near-Earth asteroid (6053) during its long-lasting apparition from July 1995 to February 1996. Nineteen R lightcurves were obtained at intervals not exceeding 36 days. The derivation of the asteroid's spin vector is based on a new implementation of the epoch method. The times of minima of the second harmonics of the Fourier series fits to the lightcurves are taken as the reference times. The most probable pole solution obtained is (175 degrees, -9 degrees) in J2000 ecliptic coordinates, with formal errors of 5 degrees and 3 degrees, respectively. The sidereal rotation period is 2.573419 +/- 0.000014 hr. There exists another, less probable solution of (359 degrees, -26 degrees, 2.573986 hr), which we cannot rule out with certainty; however, it gives also a poorer mean magnitude-aspect dependence than that for the first, most probable solution; this leads us to conclusion that the most probable solution is the true one. The shape of the asteroid can be approximated by a triaxial ellipsoid similar to an oblate spheroid, with ratios of its major axes a/b = 1.08 +/- 0.04 and b/c approximate to 1.5 or greater. Combining thermal observations made on 1995 August 12 with the visual photometric results, a range of geometric albedo p(v) of 0.11-0.25 is obtained together with a mean equatorial diameter of 3.3 +/- 0.6 km. The derived range of albedo and the measured colors (V - R = 0.48 +/- 0.02, R - I = 0.35 +/- 0.02, and B - V = 0.99 +/- 0.05) are consistent with an S-type classification. Taking a geometric albedo of 0.16 typical for this class, the axes of the ellipsoid best approximating the asteroid's shape are 2a = 3.5 km, 2b = 3.2 km, and 2c approximate to 2 km. The high power in the first harmonic observed in the lightcurves is due to a surface irregularity (deviation from the ellipsoid figure), rather than a hemispherical albedo variegation. (C) 1997 Academic Press.
