We present coupled chemical-microphysical models for the formation, growth, and physical properties of the jovian polar haze based on a gas-phase photochemical model for the auroral regions developed by A. S. Wong et al. (2000, Astrophys. J. 534, L215-217). In this model, auroral particle precipitat
A tropical haze band in Titan’s stratosphere
✍ Scribed by R. de Kok; P.G.J. Irwin; N.A. Teanby; S. Vinatier; F. Tosi; A. Negrão; S. Osprey; A. Adriani; M.L. Moriconi; A. Coradini
- Publisher
- Elsevier Science
- Year
- 2010
- Tongue
- English
- Weight
- 476 KB
- Volume
- 207
- Category
- Article
- ISSN
- 0019-1035
No coin nor oath required. For personal study only.
📜 SIMILAR VOLUMES
By comparing observations from the Cassini imaging system, UV spectrometer, and Huygens atmospheric structure instrument, we determine an apparent radius of ∼40 nm, an imaginary index <0.3 at 187.5 nm and a number density of ∼30 particles cm -3 for the detached haze layer at 520 km in Titan's mesosp
During the 1981 Voyager encounter, Titan's stratosphere exhibited a large thermal asymmetry, with high northern latitudes being colder than comparable southern latitudes. Given the short radiative time constant, this asymmetry would not be expected at the season of the Voyager observations (spring e
at a spectral resolution of λ/ λ ≈ 10 6 , at wavelength 11.7-11.9 µm using the Goddard Infrared Heterodyne Spectrometer at the NASA Infrared Telescope Facility on Mauna Kea, Hawaii. The ethane mole fraction is determined to be (8.8 ± 2.2) × 10 -6 (68.3% confidence limits, "1σ "), averaging the retri