Forming the Dusty Ring in HR 4796A

Abstract

We describe planetesimal accretion calculations for the dusty ring observed in the nearby A0 star HR 4796A. Models with initial masses of 10-20 times the minimum mass solar nebula produce a ring of width 7-15 AU and height 0.3-0.6 AU at 70 AU in roughly 10 Myr. The ring has a radial optical depth of 1. These results agree with limits derived from infrared images and from the excess infrared luminosity.

6 pages, including 2 figures and 1 table; ApJ Letters, in press

References in corpus (2)

• Accretion in the Early Kuiper Belt II. Fragmentation
• NICMOS Observations of the Pre-Main-Sequence Planetary Debris System HD 98800

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• Stellar encounters as the origin of distant solar system objects in highly eccentric orbits
• Detecting the Dusty Debris of Terrestrial Planet Formation
• STIS Imaging of the HR 4796A Circumstellar Debris Ring
• The Inner Rings of Beta Pictoris
• Outer edges of debris discs: how sharp is sharp?
• Gravitational Stirring in Planetary Debris Disks
• Collisional Cascades in Planetesimal Disks I. Stellar Flybys
• Speckle Suppression Through Dual Imaging Polarimetry, and a Ground-Based Image of the HR 4796A Circumstellar Disk
• Dusty Rings: Signposts of Recent Planet Formation
• Planet Formation in the Outer Solar System
• A Resolved Debris Disk around the G2V star HD 107146
• Modeling the Infrared Emission from the HD 141569A Disk
• Adaptive Optics Imaging of the AU Microscopii Circumstellar Disk: Evidence for Dynamical Evolution
• Modeling the Infrared Emission from the HR 4796A Disk
• Formation of Narrow Dust Rings in Circumstellar Debris Disks
• Complex Organic Materials in the HR 4796A Disk?
• Regarding the Accretion of 2003 VB12 (Sedna) and Like Bodies in Distant Heliocentric Orbits
• The `Second Parameter': A Memory from the Globular Cluster Formation Epoch
• The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) III: The vertical structure of debris disks