First Detection of a Dust Disk around Iota Horologii, a Southern Star Orbitted by an Extrasolar Giant Planet

Details First Detection of a Dust Disk around Iota Horologii, a Southern Star Orbitted by an Extrasolar Giant Planet First Detection of a Dust Disk around Iota Horologii, a Southern Star Orbitted by an Extrasolar Giant Planet

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.6533p&link_type=abstract

American Astronomical Society, DPS Meeting #32, #65.33; Bulletin of the American Astronomical Society, Vol. 32, p.1646

Physics

Optics

1

Scientific paper

The link between the presence of debris dust disks (Vega phenomenon) and planetary formation is still unclear; are they: excluding children, siamese twins, or just casual neighbours? Recenly, Trilling et al. (1999), thanks to coronograph observations in the Northern hemisphere, showed that 3 out of 6 stars with known planetary companions harbour a tenuous dust disk, probably some precursors to the analogues of our Solar System Kuiper belt and zodiacal disk. We have started to conduct a similar program in the southern hemisphere at the ESO 3.6m telescope using the adaptive optics system ADONIS. H band images taken in coronographic mode during good observing conditions reveal the presence of a tenuous dust disk around the star Iota Horologii. This star is know to have a planetary companion of 2.26 M.sin i Jupiter masses on a 1 AU orbit, revealed by radial velocities analysis. The ADONIS images show that the disk has an inclination with a tilt angle of 40 degrees with respect to the edge-on configuration. This information allows to remove the degeneracy on the estimation of the mass of the planet due to the unknown inclination of the orbit. Taking this value into account, we find that the planet mass is 3.41 Jupiter masses. In our ADONIS observations, the disk extends 3.7 arcsec from the star, i.e. about 65 AU taking into account the distance of 17 parcsecs of this system. Modelling of light scattering by dust particles are shown and compared to the observations in order to deduce the disk density profile. This density profile is compared to previous results on disks around Beta Pic and HD 100546.

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