Astronomy and Astrophysics, volume 603A, 123-123 (2017/7-1)
Dust in brown dwarfs and extrasolar planets. V. Cloud formation in carbon- and oxygen-rich environments.
HELLING C., TOOTILL D., WOITKE P. and LEE G.
Abstract (from CDS):
Context. Recent observations indicate potentially carbon-rich (C/O>1) exoplanet atmospheres. Spectral fitting methods for brown dwarfs and exoplanets have invoked the C/O ratio as additional parameter but carbon-rich cloud formation modeling is a challenge for the models applied. The determination of the habitable zone for exoplanets requires the treatment of cloud formation in chemically different regimes.
Aims. We aim to model cloud formation processes for carbon-rich exoplanetary atmospheres. Disk models show that carbon-rich or near-carbon-rich niches may emerge and cool carbon planets may trace these particular stages of planetary evolution.
Methods. We extended our kinetic cloud formation model by including carbon seed formation and the formation of C[s], TiC[s], SiC[s], KCl[s], and MgS[s] by gas-surface reactions. We solved a system of dust moment equations and element conservation for a prescribed Drift-Phoenix atmosphere structure to study how a cloud structure would change with changing initial C/O0=0.43...10.0.
Results. The seed formation efficiency is lower in carbon-rich atmospheres than in oxygen-rich gases because carbon is a very effective growth species. The consequence is that fewer particles make up a cloud if C/O0>1. The cloud particles are smaller in size than in an oxygen-rich atmosphere. An increasing initial C/O ratio does not revert this trend because a much greater abundance of condensible gas species exists in a carbon-rich environment. Cloud particles are generally made of a mix of materials: carbon dominates if C/O0>1 and silicates dominate if C/O0<1. A carbon content of 80-90% carbon is reached only in extreme cases where C/O0=3.0 or 10.0.
Conclusions. Carbon-rich atmospheres form clouds that are made of particles of height-dependent mixed compositions, sizes and numbers. The remaining gas phase is far less depleted than in an oxygen-rich atmosphere. Typical tracer molecules are HCN and C2H2 in combination with a featureless, smooth continuum due to a carbonaceous cloud cover, unless the cloud particles become crystalline.
© ESO, 2017
astrobiology - astrochemistry - planets and satellites: gaseous planets - planets and satellites: atmospheres - methods: numerical - methods: numerical
Paragraph 1. HD 8988 is a misprint for HR 8799. Paragraph 6. HD 189744 is a misprint for HD 189733.
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