Computer Science
Scientific paper
Feb 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..459f&link_type=abstract
NOAO Proposal ID #2007A-0459
Computer Science
Scientific paper
Debris disks consist of circumstellar dust grains that are freshly produced through the attrition of planetesimals around the star. Study of these disks improves our understanding of the evolution of circumstellar material over the stars' main sequence lifetimes. They provide a record of the processes governing planet formation. Moreover, the disks' architectures can reveal the presence of planets through their gravitational signatures. The edge-on disk around the A0V star HD 32297 was recently imaged in scattered light in the near IR (Schneider et al. 2005) and visible (Kalas 2005). In September 2006, we resolved thermal emission from the dust disk with Gemini/Michelle. These observations suggest an inner edge to the parent body distribution at 65 AU. Further, these observations hint at slight asymmetries in the brightness distribution. Asymmetric brightness and displacement of dust lobes can be due to unseen planetary perturbers (Wyatt et al. 1999), as suggested for Fomalhaut's dust ring (Holland et al. 2003; Kalas et al. 2005; Quillen 2006). We propose to use Gemini/Michelle to obtain deeper images of HD 32297's thermal emission at high spatial resolution (N' band), in order to quantify the level of asymmetry in the disk and fully determine its spatial extent. We will further constrain the temperature structure of the disk by imaging at longer wavelengths (Qa band). Finally, we will use low-resolution spectra in the 10 micron region to measure the composition of the disk material. These observations will inform our understanding of the evolution of disk material throughout the planet building phase.
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