Long slit Spectropolarimetry of Jupiter and Saturn

TL;DR

This study presents detailed spectropolarimetric measurements of Jupiter and Saturn, revealing high limb polarization linked to haze particles and distinct polarization behaviors across different regions and wavelengths, including new features on Saturn.

Contribution

First comprehensive ground-based spectropolarimetry of Jupiter and Saturn covering 5200-9350 Å, with modeling of haze particles explaining observed polarization features.

Findings

Jupiter's polar limb polarization reaches +11.5% at 6000 Å.

Saturn's polarization is lower and decreases with wavelength.

A new strong polarization feature near Saturn's equator was observed.

Abstract

We present ground-based limb polarization measurements of Jupiter and Saturn consisting of full disk imaging polarimetry for the wavelength 7300 A and spatially resolved (long slit) spectropolarimetry covering the wavelength range 5200 to 9350 A. For the polar region of Jupiter we find for wl=6000 A a very strong radial polarization with a seeing corrected maximum of about +11.5% in the South and +10.0% in the North. Our model calculations demonstrate that the high limb polarization can be explained by strongly polarizing (p~1.0), high albedo (omega~0.98) haze particles with a scattering asymmetry parameter of g~0.6 as expected for aggregate particles. The deduced particle parameters are distinctively different when compared to lower latitude regions. The spectropolarimetry of Jupiter shows a decrease in the polar limb polarization towards longer wavelengths and a significantly enhanced polarization in strong methane bands when compared to the adjacent continuum. For lower latitudes the fractional polarization is small, negative, and it depends only little on wavelength except for the strong CH4-band at 8870 A. The South pole of Saturn shows a lower polarization (p~1.0-1.5%) than the poles of Jupiter. The spectropolarimetric signal for Saturn decrease rapidly with wavelength and shows no significant enhancements in the fractional polarization in the absorption bands. These properties can be explained by a vertically extended stratospheric haze region composed of small particles <100nm. In addition we find a previously not observed strong polarization feature (p=1.5-2.0%) near the equator of Saturn. The origin of this polarization signal is unclear but it could be related to a seasonal effect.