Unified Model Photospheres for Ultracool Dwarfs of the Types L and T

Details Unified Model Photospheres for Ultracool Dwarfs of the Types L and T Unified Model Photospheres for Ultracool Dwarfs of the Types L and T

2001-03-23

arxiv.org/abs/astro-ph/0103395v1

Astronomy and Astrophysics

Astrophysics

18 pages, 6 figures, Proceedings of the IAU Workshop on "Ultracool Dwarfs: Surveys, Properties and Spectral Classification" (A

Scientific paper

We show that the two groups of ultracool dwarfs classified as L and T types can be understood as a temperature effect in a unique sequence of the model photospheres in which dust always exists but only in the restricted region deep in the photosphere. Under the high density of the photospheres of cool dwarfs, dust forms easily at the condensation temperature T_cond (about 2000 K), but the dust will soon grow larger than the critical radius r_cr at the critical temperature T_cr (about 1800 K). The large dust grains with r > r_cr will soon segregate from the gas and precipitate below the photosphere. For this reason, dust exists only in the limited region of T_cr < T < T_cond in the photo- sphere which we referred to as an active dust zone, and this means that a cloud layer is formed deep in the photosphere rather than in the cooler surface region. With the simple assumption that only small dust grains (r < r_cr) can be sustained in the photosphere, a self- consistent non-grey model photosphere in radiative-convective equilibrium can be developed without any other ad-hoc assumption. We show that the spectra and colours of L (the cloud layer appears in the optically thin region) and T (the dust cloud is situated too deep to be observable) dwarfs can consistently be reproduced by a single grid of our unified model photospheres.

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