Computer Science
Scientific paper
Apr 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998exdu.work..275j&link_type=abstract
Exozodiacal Dust Workshop, p. 275
Computer Science
Stellar Envelopes, Dynamic Models, Trapped Particles, Planets, Detection, Poynting-Robertson Effect, Brightness, Size Distribution
Scientific paper
Planets embedded in circumstellar disks trap dust particles, spiraling towards the central star due to Poynting-Robertson drag, into outer mean motion resonances. The resonant trapping leads to a local enhancement of the dust creating a circumstellar ring at the semimajor axis of the planet. The number density of particles in the ring depends upon the drag rate of the particles and the mass of the planet. Such a ring formed by asteroidal particles has been detected around the Earth. The structure of the ring depends upon the circumstellar radiation environment, the mass of the star and the planet, the number density of dust in the disk, and the size distribution of the particles. We have developed models of resonant rings at different orientations from edge-on, (incl = 0 deg) to face-on, (incl = 90 deg) using a dynamic model of the resonant ring at 1 AU associated with the Earth. A composite image of a model disk and a ring has also been created using a simple background dust distribution. The integrated brightness profiles in, and normal to, the plane of the disk deviate significantly from a smooth scan and show the signature of a planet. The following characteristics of Resonant Rings provide evidence for the presence of a planet embedded in a stellar disk: (1) Sharp features that occur in pairs in the brightness profiles of the disk is the typical signature for a ring and, consequently, for the presence of a planet; (2) The ring is rotationally asymmetric and locked to the motion of the planet. Hence, time variations in azimuthal brightness, particularly in face-on, disks (incl >> 90 deg), is a measure of the period of the planet; and (3) For massive planets (mp > mass of Jupiter), the fraction of particles trapped can be high enough to halt the flow of particles to the star, thereby creating a gap in the disk.
Jayaraman Sumita
Lien David
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