Venus Cloud Particle Size Distributions and Altitudes from IRTF/SpeX Spectral Image Cubes

Details Venus Cloud Particle Size Distributions and Altitudes from IRTF/SpeX Spectral Image Cubes Venus Cloud Particle Size Distributions and Altitudes from IRTF/SpeX Spectral Image Cubes

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.6009b&link_type=abstract

American Astronomical Society, DPS meeting #41, #60.09

Computer Science

Databases

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Absorption of infrared radition at 1.10, 1.18, 1.31, 1.74, and 2.3 μm due to molecular gas electronic transitions is minimal through the Venus atmosphere. Blackbody radiation from the surface and deep atmosphere, observed on the night side, is therefore mostly affected by cloud aerosols. Ratios of the observed fluxes in each of these windows provide information on the scatterers’ sizes. Altitudes can be derived by the use of forward modeling to simulate the observed temperatures and fluxes.
We use IRTF/SpeX spectra of the nightside of Venus we obtained in July and September 2007, simultaneous with Venus Express VIRTIS observations of the southern hemisphere at the same wavelengths. By allowing the 60” spectrometer slit to drift across Venus’ night side over approximately 15 minutes, we acquired spectral image cubes comprised of about 100 spectra, from 0.8 to 2.5 μm with a spectral resolution of R 400.
We use a multiple scattering line-by-line radiative transfer code and the HITRAN 2004 and HITEMP databases to calculate the fluxes in each window for a range of cloud structure and altitudes. Ratios of fluxes in each of the windows that are diagnostic of cloud particle distributions are compared with these ratios in our spectral image cubes. By obtaining a least squares best fit to the data, we produce maps of particle sizes and altitudes of the Venus clouds.

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