Ballard is a member of the Phocaea family (701).[3] It orbits the Sun in the inner asteroid belt at a distance of 1.83–2.98 AU once every 3 years and 9 months (1,360 days; semi-major axis of 2.4 AU). Its orbit has an eccentricity of 0.24 and an inclination of 23° with respect to the ecliptic.[2] The body's observation arc begins with a precovery taken at Palomar in September 1988, just four weeks prior to its official discovery observation.[1] Ballard is not a Mars-crosser, since its aphelion is larger than 1.67 AU.[2]
In July 2010, a rotational lightcurve of Ballard was obtained from two nights of photometric observations in the R-band by Italian astronomer Albino Carbognani at the OAVdA Observatory (B04) in Italy. Lightcurve analysis gave a tentative rotation period of at least 10 hours with a brightness amplitude of more than 0.25 magnitude (U=2-).[7]
The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.23 – derived from the family's largest member, 25 Phocaea – and calculates a diameter of 6.65 kilometers based on an absolute magnitude of 13.1.[4]
^ abcdMainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode:2016PDSS..247.....M. Retrieved 25 September 2018.
^ abCarbognani, Albino (January 2011). "Lightcurves and Periods of Eighteen NEAs and MBAs". The Minor Planet Bulletin. 38 (1): 57–63. Bibcode:2011MPBu...38...57C. ISSN1052-8091.
^ abMasiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID46350317.