Thickness of Saturn’s B ring as derived from seasonal temperature variations measured by Cassini CIRS

Abstract Structural and thermal properties of Saturn’s B ring and its particles are derived from orbital and seasonal temperatures variations observed by the Cassini CIRS spectrometer between 2004 and 2009 equinox. Our multiscale thermal model (Ferrari, C., Reffet, E. [2013]. Icarus 223, 28–39), which assumes negligible heat transfer by vertical motion of particles in dense rings, is adjusted to the data. Most observations were focused on the center of the B ring, at 105,000 km from Saturn. A very good fit is obtained for conductive particles embedded in a moderately conductive ring medium. Assuming a bulk composition of water ice, the thermal inertia of particles is found to be Γ 1 = 160 – 200 J / m 2 / K / s 1 / 2 and to vary with seasons as part of the heat transfer is radiative, then temperature-dependent. For the same reason, the thermal inertia of the ring, Γ 0 , varies with seasons, between 30 and 35  J / m 2 / K / s 1 / 2 . It is very comparable to the thermal inertia of icy satellite surfaces. The porosity of particles p 1 found to fit this thermal inertia is very high (0.93) and may emphasize an inappropriate modeling of particles by an effective porous medium. The ring filling factor is fairly high, D = 0.34 ± 0.01 , but stays typical of a compact medium and compatible with the output of numerical simulations of dense ring dynamics. The thickness of the B ring at 105,000 km from Saturn is estimated at H S = 2.2 ± 0.2  m. The observed correlation of its optical depth with the thermal gradient between lit and unlit sides is easily reproduced by the model if the radial variations in optical depth are due to varying thickness H S ( a ) with constant filling factor. This thickness varies between 1 and 3 m across the B 2 , B 3 and B 4 regions. It is thinner than the neighboring C ring and Cassini Division. This can be understood as a consequence of self-gravity. The ring surface mass density Σ = ( 1 - p 1 ) ρ 0 DH S ( a ) derived from these structural parameters is too low for a self-gravitating ring, due to the high porosity found. But its radial variations, if deduced from coupling H S ( a ) with known aspect-ratios H / λ of self-gravity wakes, range between 300 in the inner B ring and most certainly exceed 1000  kg / m 2 in the B 3 ring, values compatible with a self-gravitating ring. The inferred minimum total mass of Saturn's rings is M R = 1.4 ± 0.2 · 10 19  kg, close to the mass expected for a viscous disk evolving over the age of the Solar System and compatible with current higher estimates.