In November 2017, a rotational lightcurveofLova was obtained from photometric observations by Tom Polakis at the Command Module Observatory (V02) in Arizona. Lightcurve analysis gave a well-defined rotation periodof41.118±0.011 hours with a brightness variation of 0.28±0.01magnitude (U=3).[10] While not being a slow rotator, which have periods of 100 or more hours, Lova's period is significantly longer than the vast majority of asteroids, which rotate within 2.2 to 20 hours once around their axis.
A lower-rated lightcurve by French amateur astronomer Laurent Bernasconi gave a similar period of 41.3±0.2 hours with a higher amplitude of 0.40±0.01 magnitude, indicative of an elongated shape (U=2).[13] The results supersede a period determination with a lower limit of 24 hours and amplitude of at least 0.11 magnitude by Brian Warner at his Palmer Divide Observatory in Colorado from November 1999 (U=2). In 2006, Warner revised his photometric data, though with no notable improvement or change for this asteroid.[14][15][a]
According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Lova measures (50.692±0.191), (52.47±1.5) and (55.45±0.73) kilometers in diameter and its surface has an albedo of (0.056±0.006), (0.0524±0.003) and (0.048±0.002), respectively.[7][8][9] The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, a low albedo of 0.0524 and a diameter of 52.47 kilometers based on an absolute magnitude of 10.22.[12] Alternative mean-diameter measurements published by the WISE team include (49.742±17.318 km), (50.057±12.98 km), (51.194±0.567 km) and (59.77±19.19 km) with corresponding albedos of (0.0400±0.02), (0.0400±0.0411), (0.0550±0.0072) and (0.03±0.01).[5][12]
Two asteroid occultations, observed on 5 April 2006 and 12 July 2007, gave a best-fit ellipse dimension of (52.0 × 52.0) and (43.3 × 64.3) kilometers, respectively, with the latter being the better rated one.[5] These timed observations are taken when the asteroid passes in front of a distant star.[5]
^Lightcurve plot of 868 Lova, Palmer Divide Observatory, B. D. Warner (1999). Rotation period larger than 24 hours with a brightness amplitude of more than 0.11 mag. Quality code of 2. Summary figures for (868) Lova at the LCDB. The result has been superseded by a period of 41.118 hours.
^ abcMasiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121.
^ abcUsui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
^Schmadel, Lutz D. (2007). "Appendix 11 – Minor Planet Names with Unknown Meaning". Dictionary of Minor Planet Names – Fifth Revised and Enlarged revision. Springer Berlin Heidelberg. pp. 927–929. ISBN978-3-540-00238-3.