?The slope of the tholin albedo in the blue is similar to that required by the observations at the highestaltitudes. However, the curve for these tholins continues to increase toward longer wavelengths to 1600 nm, while the observations require a decrease longward of about 900 nm. It will be interesting to compare the Titan albedos to measurements for other types of tholin products.
I should do this. I can compare a bunch of different set to match albedo to constraint especially the ni.
The strong linear polarization observed in both red and blue wavelengths requires that the monomers out of which the aggregate particles are built have radii of 0.05 mm or less. The size of the SA requires that the aerosols consist of some 3000 monomers (to within a factor of 2).
The single-scattering phase function is constrained by the SA measurements near the sun, and has sufficiently strong forward scattering to fit the brightness of Titan seen at large phase angles relative to smaller phase angles (Rages et al., 1983).
Does this mean that, the ratio of forward scattering angles observed in DISR to low phase angles observed during an occultation will constraint the aerosol monomer numbers?
Important Information from various reference papers
I/F profile, plane parallel atmnosphere & phase functions
For our initial analysis, each high-phase-angle frame has been characterized by a single number--the maximum value of the normalized scattered intensity I/F along a radial scan (A normally illuminated, perfectly reflecting Lambert surface gives I/F = 1.) We have chosen to use only the maximum I/F value, because the shape of the intensity profile interior to the maximum I/F is almost totally insensitive to changes in the single-scattering phase function. The shape of the intensity profile is, however, sensitive to departures from plane parallel geometry, while our calculations show that the maximum I/F generally is not affected to any pronounced degree. \cite{Rages_1983}
Why Single Scattering prop. important
Measurements of the size and shape of the particles permit thesingle scattering, and thus multiple scattering of solar radiation in the atmosphere to be modeled. Such models are necessary to cre- ate models of the radiative net fluxes and the profiles of solar heat- ing in the atmosphere to give the radiative forcing for atmospheric dynamics.
From \cite{Tomasko_2009}
Fig21. The shapes of the single-scattering intensity phase functions used for the blue models. The peaks for scattering angles less than 9° are from the appendix of Tomasko et al. (2008) while the curves for angles greater than 9° are smoothly mated to the Henyey–Greenstein functions used in Tomasko et al. (2008) to fit the blue Solar Aureole measurements at a wide range of angles from the Sun.