One Hundred Years of Venus Polarimetry: PICSARR Observations of the Phase Curves

TL;DR

This study presents a century of Venus polarization observations, comparing new high-precision data with historical models, revealing polarization variability and polar region differences likely due to Rayleigh scattering and cloud-top height variations.

Contribution

The paper provides updated polarization measurements of Venus, validates and extends past models with modern radiative transfer codes, and highlights polarization differences in ultraviolet wavelengths indicating atmospheric heterogeneity.

Findings

Good agreement with past polarization measurements and models.

Detection of polarization variability across different phases and times.

Ultraviolet polarization differences suggest heterogeneous atmospheric properties.

Abstract

We report new high-precision observations of the polarization of light scattered from the atmosphere of Venus, made 100 years after the pioneering studies by Bernard Lyot. The new observations include disk-integrated observations in a range of filters as well as imaging polarimetry. We compare the new results with past observations and models. We have reproduced the 1974 modelling of the Venus polarization by Hansen and Hovenier using modern radiative transfer codes. We show that the new models are in good agreement with the originals, and enable us to calculate the polarization for wavelengths not covered by the original study and to model the polarization distribution across the disk. The new observations are in good agreement with past determinations of the size distribution of the predominant particle mode. They agree with past studies in showing variability of the phase curve between synodic cycles and also polarization variability on short timescales, particularly at higher phase angles (crescent phases). Imaging polarimetry observations show good agreement with models for the redder wavelengths. However, observations in the ultraviolet show very different polarization behavior in the polar regions (within about 30 degrees of the north and south poles). The simplest explanation of this result is that there is a larger Rayleigh scattering component in the polar regions than in the equatorial and mid-latitudes and this could be explained by a lower cloud-top height in agreement with previous spacecraft observations. These ultraviolet polarization observations are inconsistent with horizontally homogeneous atmospheric models.