Ji-Wei Xie, Alexis Brandeker, Yanqin Wu
The metallic gas associated with the Beta Pic debris disk is believed to not be primordial, but arise during the destruction of dust grains. Recent observations have shown that carbon and oxygen in this gas are exceptionally overabundant compared to other elements, by some 400 times. We study the origin of this enrichment under two opposing hypothesis, preferential production, where the gas is produced with the observed unusual abundance, and preferential depletion, where the gas evolves to the observed state from an original solar abundance under a number of dynamical processes. We include in our study the following processes: radiative blow-out of metallic elements, dynamical coupling between different species, and viscous accretion onto the star. We find that, if gas viscosity is sufficiently low (the conventional alpha parameter <1e-3), differential blow-out dominates. While gas accumulates gradually in the disks, metallic elements subject to strong radiation forces, such as Na and Fe, deplete more quickly than C and O, naturally leading to the observed overabundance of C and O. On the other hand, if gas viscosity is high (alpha>1e-1, as expected for this largely ionized disk), gas is continuously produced and viscously accreted toward the star. This removal process does not discriminate between elements so the observed overabundance of C and O has to be explained by a preferential production that strongly favors C and O to other metallic elements. One such candidate is photo-desorption off the grains. We compare our calculation against all observed elements (~10) in the gas disk and find a mild preference for the second scenario, based on the abundance of Si alone. If true, Beta Pic should still be accreting at an observable rate, well after its primordial disk has disappeared.
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http://arxiv.org/abs/1204.4087
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