In February 2008, a rotational lightcurve of Kovacia was obtained from photometric observations by a collaboration of French and Italian amateur astronomers including René Roy, Silvano Casulli, François Colas, Arnaud Leroy, Federico Manzini, Christophe Demeautis and Jean-François Coliac.
Lightcurve analysis gave a well-defined rotation period of 8.6772±0.0001 hours with a high brightness variation of 0.86±0.02 magnitude, indicative of a non-spherical, elongated shape (U=3).
The result supersedes a previous observation by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station (A12) from November 2006, that determined a lower limit of 6 hours (U=1+).
Due to observed mutual occultation and eclipsing events, the collaboration of astronomers strongly suspect Kovacia to be a binary asteroid with a satellite orbiting it every 31.9580±0.0005 days.
However, no follow-up observations have been published.
As of March 2020, this asteroid is neither listed at Johnston's Archive nor has it any kind of binary status in the Lightcurve Data Base.

In 2016, a modeled lightcurve gave a concurring sidereal period of 8.67807±0.00002 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys (950).
The study also determined two spin axes of (200.0°, −44.0°) and (38.0°, −50.0°) in ecliptic coordinates (λ, β).
In February 2008, a rotational lightcurve of Kovacia was obtained from photometric observations by a collaboration of French and Italian amateur astronomers including René Roy, Silvano Casulli, François Colas, Arnaud Leroy, Federico Manzini, Christophe Demeautis and Jean-François Coliac. Lightcurve analysis gave a well-defined rotation period of 8.6772±0.0001 hours with a high brightness variation of 0.86±0.02 magnitude, indicative of a non-spherical, elongated shape (U=3). The result supersedes a previous observation by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station (A12) from November 2006, that determined a lower limit of 6 hours (U=1+). Due to observed mutual occultation and eclipsing events, the collaboration of astronomers strongly suspect Kovacia to be a binary asteroid with a satellite orbiting it every 31.9580±0.0005 days. However, no follow-up observations have been published. As of March 2020, this asteroid is neither listed at Johnston's Archive nor has it any kind of binary status in the Lightcurve Data Base.
In 2016, a modeled lightcurve gave a concurring sidereal period of 8.67807±0.00002 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys (950). The study also determined two spin axes of (200.0°, −44.0°) and (38.0°, −50.0°) in ecliptic coordinates (λ, β).
867 Kovacia