The origin of variability in a hot-Jupiter

Details The origin of variability in a hot-Jupiter The origin of variability in a hot-Jupiter

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010sptz.prop70100s&link_type=abstract

Spitzer Proposal ID #70100

Computer Science

Scientific paper

We will determine (1) if the variability, detected by Spitzer/IRS in the dayside emission spectrum of the hot-Jupiter HD 189733b via the secondary eclipse method, is accompanied by correlated variability in the primary eclipse and (2) place further constraints on the global energy budget. The primary eclipse (a transmission measurement) primarily probes composition while the secondary eclipse (an emission measurement) probes a combination of composition and temperature. By testing for correlated variations in the primary and secondary eclipse depth, we will establish whether variability present in HD 189733b is primarily due to changes in temperature, changes in composition (such as inter-conversion of carbon monoxide into methane), or some combination of the two. We will compare our multi-epoch measurements of the primary/secondary eclipse depth ratio at 3.6 microns to the existing multi-epoch measurements of the primary/secondary eclipse depth ratio at 8 microns (Agol et al. 2010); our proposed measurements will place additional constraints on the global energy budget of the planet. We will also use ground-based 3.1-4.1 micron spectroscopy, of both the primary and secondary eclipse events, to provide additional modeling constraints for interpreting the IRAC 3.6 micron photometry measurements.

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