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SUMMARY:DISEQUILIBRIUM CHEMISTRY SIGNATURES WITH JWST\, AND TOWARDS THE CO
 NSISTENT MODELLING OF HAZE IN EXOPLANET ATMOSPHERES  - Sarah Blumenthal (E
 xeter)
DTSTART:20190430T150000Z
DTEND:20190430T160000Z
UID:TALK121945@talks.cam.ac.uk
CONTACT:Richard Booth
DESCRIPTION:\nWhen will the James Webb Space Telescope launch? This questi
 on will not be answered in this talk\, but we take a rough first look at n
 arrowing the parameter space in terms of chemical observation with the Jam
 es Webb Space Telescope (Blumenthal et al.\, 2018) We look at 3 planet cas
 es that mimic a range of planetary radius and equilibrium temperature. We 
 link and compare two types of chemistry models from Venot et al. (2012)—
 thermochemical equilibrium and chemical kinetics with photochemistry —wi
 th a 1D radiative transfer model (Cubillos et al.\, in preparation). We th
 en link this output to the JWST imulator\, PandExo (Batalha et al.\, 2017)
 .  We find some observable differences between the two chemical models fro
 m 4 to 5 microns due to the abundances of CO\, CO2\, and H2O. Thus\, we pr
 escribe a ‘sweet spot’ of planetary mass\,\ntemperature\, and metallic
 ity that would be most fruitful for high-resolution characterization with 
 JWST.  As Blumenthal et al. (2018) used a forward modeling approach with t
 he chemistry of Venot et al.\, (2012)\, we begin to explore the applicatio
 n of different chemical schemes in a 1D self-consistent radiative-convecti
 ve and chemistry atmospheric code\, ATMO (Tremblin et al.\, 2015).  We imp
 lement a larger hydrocarbon chemical network (Venot et al.\, 2015) into AT
 MO\, with the goal of modeling haze precursors and their feedback on the s
 tructure of the atmosphere.  I will present the benchmark of this work and
 \nadditionally\, some preliminary work on implementation of a sulfur chemi
 cal network (Zahnle et al.\, 2016) into ATMO. 
LOCATION:Martin Ryle Seminar Room\, Kavli Institute
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