In 2006, a debris field was discovered in orbit around this star using infrared observations by the Spitzer Space Telescope. This debris is thought to be an asteroid belt. The measured temperature of the debris is 110 K, which places it in an orbit between 4 and 6 AU from the star, or about the same distance where Jupiter orbits the Sun.[12] This debris disk may have been created by the breakup of a single, 100 km diameter planetesimal through a collision.[13] The star system does not show any excess emission at 70 μm, indicating it does not have a cold outer dust disk.[14]
The star was examined for the presence of an extrasolar planet with a mass in the range 2-10 Jupiter masses and an orbital distance of 3-15.5 AU. Instead, in 2007, a close stellar companion was likely discovered. This object is separated from the primary by 0.15 arcseconds, making it unlikely to be a background object.[15]
This star has been proposed as a member of the Tucana-Horologium association (Tuc-Hor), a stream of young stars with a common motion through space. The Tuc-Hor association is about 30 million years old.[16][17] The space velocity components of this star are [U, V, W] = [−0.6, −16.3, 5.0] km/s.[11] It is orbiting the Milky Way galaxy with an orbital eccentricity of 0.06, with a distance that varies from 7.11−8.01 kpc of the galactic core. The inclination of its orbit carries it as far as 90 parsecs above the galactic plane.[6]
^Greaves, Jane; et al. (May 2007). "The composition of debris around HD 12039: water from asteroids?". Spitzer Proposal ID #40310: 40310. Bibcode:2007sptz.prop40310G.
^Klahr, Hubert; Brandner, Wolfgang (2006). Planet formation: theory, observations and experiments. Cambridge University Press. p. 28. ISBN978-0-521-86015-4.
