In 2006, a debris field was discovered in orbit around this star usinginfrared observations by theSpitzer Space Telescope. This debris is thought to be anasteroid belt. The measured temperature of the debris is 110 K, which places it in an orbit between 4 and 6AU from the star, or about the same distance whereJupiter orbits the Sun.[12] Thisdebris disk may have been created by the breakup of a single, 100 km diameterplanetesimal through a collision.[13] The star system does not show anyexcess emission at 70 μm, indicating it does not have a cold outer dust disk.[14]
The star was examined for the presence of anextrasolar planet with a mass in the range 2-10 Jupiter masses and an orbital distance of 3-15.5AU. Instead, in 2007, a close stellar companion was likely discovered. This object is separated from the primary by 0.15arcseconds, making it unlikely to be a background object.[15]
This star has been proposed as a member of theTucana-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] Thespace velocity components of this star are[U, V, W] =[−0.6, −16.3, 5.0] km/s.[11] It is orbiting theMilky Way galaxy with anorbital eccentricity of 0.06, with a distance that varies from 7.11−8.01 kpc of the galactic core. Theinclination 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.
