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Silicate, ruby, opal – Why gas giants keep their jewels in the atmosphere

Published online by Cambridge University Press:  01 October 2007

Christiane Helling*
Affiliation:
SUPA, School of Physics & Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, Scotland, UK email: Christiane.Helling@st-andrews.ac.uk
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Abstract

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Giant gas-planets - and brown dwarfs - form dust clouds in their atmospheres which are made of a variety of gemstone-like and possible liquid materials. Our theoretical approach, where we calculate homogeneous nucleation, heterogeneous growth/evaporation, gravitational settling, and element consumption for composite dust grains, allows to access the evolution of the dust complex in the cloud, and hence also the elements remaining in the gas phase. The cloud formation process is imprinted into these remaining elements. Following a (T, p) trajectory into the atmosphere we observe that 1. metals disappear, 2. dust forms, 3. metals re-appear, 4. dust disappears. For the first time, our kinetic cloud formation approach is coupled with an 1D atmosphere simulation and, hence, synthetic spectra can be produced based on detailed cloud micro-physics. Results are demonstrated for metal-poor gas giants and the strong influence of the dust modelling on alkali-line profile is shown.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Dehn, M. 2007, PhD Thesis, University HamburgGoogle Scholar
Dominik, C., Sedlmayr, E., Gail, H.-P. 1993, A&A 277, 578Google Scholar
Gail, H.-P., Sedlmayr, E. 1988, A&A 206, 153Google Scholar
Hauschild, P., Baron, E. 1999, JCAM 109, 41Google Scholar
Helling, Ch. 2005, eds. Kupka, Hillebrandt, 152; astro-ph/0506204Google Scholar
Helling, Ch. 2007, ASPCS, eds. Fischer, Rasio, Thorsett, Wolszczan; arXiv:0711.3730v1Google Scholar
Helling, Ch., Dehn, M., Woitke, P., Hauschildt, P. 2008, ApJL submittedGoogle Scholar
Helling, Ch., Woitke, P. 2006, A&A 455, 325Google Scholar
Helling, Ch., Woitke, P. 2004, A&A 423, 657Google Scholar
Helling, Ch., Woitke, P. & Thi, W.-F. 2008, A&A submittedGoogle Scholar
Johans, C. M. S. 2007, PhD Thesis, University HamburgGoogle Scholar
Johans, C. M. S., Helling, Ch., Woitke, P., Hauschildt, P. 2007, ASPCS, eds. Fischer, Rasio, Thorsett, WolszczanGoogle Scholar
Ludwig, H.-G., Allard, F., Hauschildt, P.H. 2006, A&A 459, 599Google Scholar
Woitle, P. 2006, A&A 460, L9Google Scholar
Woitke, P. & Helling, Ch. 2004, A&A 414, 335Google Scholar
Woitke, P. & Helling, Ch. 2003, A&A 399, 297Google Scholar