Uranus and Neptune Models
The following tables contain the latest Uranus and Neptune models provided
by the different authors below expressed in different units:
Uranus, Lellouch,,
(see plots and
explanatory note)
Uranus, Abbas,
(see plots)
Uranus, Griffin & Orton,
(see plots)
Neptune, Lellouch,
(see plots and
explanatory note)
Neptune, Abbas,
(see plots and
explanatory note)
Note that the flux densities are given per unit solid angle. The
planet's angular diameters at different dates can be found in the Astronomical
Almanac. Typical values are 3".55 (==> 2.33E-10 sr) for Uranus, and 2".22 (==>
0.912E-10 sr) for Neptune.
Model comparisons
The differences in the fluxes predicted by the different models
are typically smaller than 15%. Find here a
comparison between the different Uranus models
above.
Important note:
Currently, the LWS Relative Spectral Response
Function (RSRF) is based on the Uranus model provided by Griffin &
Orton while
the absolute flux calibration of ISOPHT at long wavelengths is based on
a combination of stars, asteroids and planets. For the planets, the Uranus
and Neptune models provided by Abbas are used.
The selection of the Griffin and Orton's model to derive the RSRF of LWS
is supported by the good agreement found between this model and
observations of Mars and other solar system objects at short wavelengths
Last update: 28-07-2000 by
Pedro Garcia-Lario