Remote Sensing Methods for Monitoring the Climates of Venus, Earth and Mars

Details Remote Sensing Methods for Monitoring the Climates of Venus, Earth and Mars Remote Sensing Methods for Monitoring the Climates of Venus, Earth and Mars

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.u34b..04c&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #U34B-04

Computer Science

Sound

0343 Planetary Atmospheres (5210, 5405, 5704)

Scientific paper

A wide range of remote sensing methods have been used to study the climates of Venus, Earth, and Mars. In some cases, techniques pioneered for Earth were subsequently used to study the climates of Venus and Mars. For example, the thermal infrared limb sounders used on NIMBUS 7 (LIMS, SAMS) and UARS (ISAMS, CLAES) were the precursors of the Mars Reconnaissance Orbiter Mars Climate Sounder (MRO MCS). In other cases, methods first used to study planetary environments, were then used to study the Earth's climate. The Pioneer Venus Orbiter Cloud Photopolarimeter (PV OCPP) was a precursor to the POLDER instruments on ADEOS and PARASOL, and the Aerosol Polarimetry Sensor (APS) on the Glory spacecraft. Similarly, hyperspectral imagers that have long been used for studying planetary environments (NIMS, VIMS, OMEGA, VIRTIS) have only recently been used for studying the Earth (EO1 Hyperion). High spectral resolution solar remote sensing methods like those being developed for measuring CO2 and other greenhouse gases, such as those on the NASA Orbiting Carbon Observatory (OCO) and the Japanese Greenhouse Gases Observing Satellite (GOSAT) provide new tools for measuring surface pressures, trace gas abundances, and the dust and ice distributions in the Martian atmosphere. Active radar and lidar sounders, like those deployed on the CloudSat and CALIPSO spacecraft, provide new methods for studying the vertical structures of the H2SO4 clouds of Venus as well as dust and ice clouds on Mars. These and other opportunities will be reviewed here.

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