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 with a width of 7-15 AU and a height of 0.3-0.6 AU at 70 AU in ∼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.
CITATION STYLE
Kenyon, S. J., Wood, K., Whitney, B. A., & Wolff, M. J. (1999). Forming the Dusty Ring in HR 4796A. The Astrophysical Journal, 524(2), L119–L123. https://doi.org/10.1086/312313
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