منابع مشابه
Dusty Rings: Signposts of Recent Planet Formation
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 du...
متن کاملTiny Molten Droplets, Dusty Clouds, and Planet Formation
Chondrules, millimeter-sized spherules that formed as rapidly-cooled molten droplets, are characteristic of chondrite meteorites. If they formed at low pressure in the solar nebula (the cloud of gas and dust surrounding the infant Sun and from which the planets formed), then they should have lost almost all their inventories of volatile elements, such as sodium, because volatile elements would ...
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 کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Oceanography
سال: 2014
ISSN: 1042-8275
DOI: 10.5670/oceanog.2014.09