Dusty Rings: Signposts of Recent Planet Formation
نویسندگان
چکیده
Many nearby stars are surrounded by a bright ring or disk of cold dust. Our calculations show that these disks and rings of dust are signposts of recent planet formation. Bright rings appear because dust associated with the formation of a planet absorbs and scatters light from the central star. The calculations explain the rings observed so far and predict that all nascent solar systems have dusty rings. Subject headings: planetary systems – solar system: formation – stars: formation – circumstellar matter
منابع مشابه
Dusty Debris Disks as Signposts of Planets: Implications for Spitzer Space Telescope
Submillimeter and near-infrared images of cool dusty debris disks and rings suggest the existence of unseen planets. At dusty but nonimaged stars, semimajor axes of associated planets can be estimated from the dust temperature. For some young stars these semimajor axes are greater than 100 as seen from Earth. Such stars are excellent targets for sensitive near-infrared imaging searches for warm...
متن کاملDusty Debris Disks as Signposts of Planets: Implications for SIRTF
Submillimeter and near-infrared images of cool dusty debris disks and rings suggest the existence of unseen planets. At dusty but non-imaged stars, semi-major axes of associated planets can be estimated from the dust temperature. For some young stars these semi-major axes are greater than an arc second as seen from Earth. Such stars are excellent targets for sensitive near-infrared imaging sear...
متن کاملDetecting the Dusty Debris of Terrestrial Planet Formation
We use a multiannulus accretion code to investigate debris disks in the terrestrial zone, at 0.7–1.3 AU around a 1 M⊙ star. Terrestrial planet formation produces a bright dusty ring of debris with a lifetime of & 10 yr. The early phases of terrestrial planet formation are observable with current facilities; the late stages require more advanced instruments with adaptive optics. Subject headings...
متن کاملStructure in the Epsilon Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron
The morphology of the ǫ Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5:3 and 3:2 exterior mean-motion resonances with a 0.3 eccentricity 10 solar mass planet at periastron at a semi-major axis of 40 AU. The morphology will differ when the planet is at apastron, in about 140 years. Moderate eccentricity planets in outer extra-solar systems will ca...
متن کاملStructure in the Epislon Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron
The morphology of the ǫ Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5:3 and 3:2 exterior mean-motion resonances with a 0.3 eccentricity 10 solar mass planet at periastron at a semi-major axis of 40 AU. The morphology will differ when the planet is at aphelion, in about 140 years. Moderate eccentricity planets in outer extra-solar systems will ca...
متن کامل