[PPS06-P02] Current status and development of Venus’ haze retrieval algorithms based on AKATSUKI observation
Keywords:Venus, haze
The Venus cloud consists of a main cloud deck at 47 – 70 km, with thinner hazes above and below. The upper haze on Venus lies above the main cloud surrounding the planet, ranging from the top of the cloud (70 km) up to as high as 90 km.
On December 7, 2015, AKATSUKI (JAXA) arrived at Venus after orbit insertion. Some instruments onboard AKATSUKI will observe characteristics of cloud and haze particles at some wavelengths.
MWP (Multi-wavelength and multi-pixel) method [M. Hashimoto et al., in revision] has been originally developed to derive Earth’s aerosol optical properties. In this study, we applied MWP method to AKATSUKI data for retrieving haze optical properties for the first time. In this presentation, a plan to application of MWP method to AKATSUKI data and first result will be introduced.
On December 7, 2015, AKATSUKI (JAXA) arrived at Venus after orbit insertion. Some instruments onboard AKATSUKI will observe characteristics of cloud and haze particles at some wavelengths.
MWP (Multi-wavelength and multi-pixel) method [M. Hashimoto et al., in revision] has been originally developed to derive Earth’s aerosol optical properties. In this study, we applied MWP method to AKATSUKI data for retrieving haze optical properties for the first time. In this presentation, a plan to application of MWP method to AKATSUKI data and first result will be introduced.