2005/11/22 by Christine H. Chen, Christine Chen, Chen, Christine H.
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0511657
15 pages, 3 figures; to appear in the ASP conference proceedings of "Frank N. Bash Symposium 2005: New Horizons in Astronomy", editors: S. Kannappan, S. Redfield, N. Drory, J. Kessler-Silacci, & M. Landriau
arxiv created 2005/11/22 · openalex publication_date 2005/11/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Debris disks are dusty, gas-poor disks around main sequence stars (Backman & Paresce 1993; Lagrange, Backman & Artymowicz 2000; Zuckerman 2001). Micron-sized dust grains are inferred to exist in these systems from measurements of their thermal emission at infrared through millimeter wavelengths. The estimated lifetimes for circumstellar dust grains due to sublimation, radiation and corpuscular stellar wind effects are typically significantly smaller than the estimated ages for the stellar systems, suggesting that the grains are replenished from a reservoir, such as sublimation of comets or collisions between parent bodies. Since the color temperature for the excess emission is typically Tgr ~ 110 - 120 K, similar to that expected for small grains in the Kuiper Belt, these objects are believe to be generated by collisions between parent bodies analogous to Kuiper Belt objects in our solar system; however, a handful of systems possess warm dust, with Tgr > 300 K, at temperatures similar to the terrestrial planets. We describe the physical characteristics of debris disks, the processes that remove dust from disks, and the evidence for the presence of planets in debris disks. We also summarize observations of infalling comets toward beta Pictoris and measurements of bulk gas in debris disks.