Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk

Details Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005natur.433..133t&link_type=abstract

Nature, Volume 433, Issue 7022, pp. 133-136 (2005).

Computer Science

67

Scientific paper

When viewed in optical starlight scattered by dust, the nearly edge-on debris disk surrounding the A5V star β Pictoris (distance 19.3pc ref. 1) extends farther than 1,450AU from the star. Its large-scale complexity has been well characterized, but the detailed structure of the disk's central ~200-AU region has remained elusive. This region is of special interest, because planets may have formed there during the star's 10-20-million-year lifetime, perhaps resulting in both the observed tilt of 4.6 degrees relative to the large-scale main disk and the partial clearing of the innermost dust. A peculiarity of the central disk (also possibly related to the presence of planets) is the asymmetry in the brightness of the `wings', in which the southwestern wing is brighter and more extended at 12µm than the northeastern wing. Here we present thermal infrared images of the central disk that imply that the brightness asymmetry results from the presence of a bright clump composed of particles that may differ in size from dust elsewhere in the disk. We suggest that this clump results from the collisional grinding of resonantly trapped planetesimals or the cataclysmic break-up of a planetesimal.

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