1. METO 637 Lesson 23

2. Titan

3. A satellite of Jupiter. Titan has a bulk composition of about half water ice and half rocky material. Although similar to the other satellites of Jupiter it is denser because it is so large that its gravity slightly compresses the interior. Titan has no magnetic field. Hence the solar wind can ionize and carry away some of the molecules from the top of the atmosphere. There is some evidence for precipitation, erosion, mechanical abrasion, and other fluvial activity. Few if any craters visible – surface must be young. However it could be that ‘oceans’ have filled some of the voids.

4. The atmosphere of Titan Has an atmosphere that is largely composed of Nitrogen. The temperature at the surface is 94.5K and the surface pressure is 1.5 bar. The instrument IRIS on Voyager detected a suite of hydrocarbons and nitrogen compounds in addition to methane. Satellite is covered by colored clouds. Clouds have been identified as arising from the gaseous organic compounds – Titan’s equivalent of photochemical smog! Clouds extend from the surface to 200 km. Above this is a thinner haze layer of aerosol particles. Heating in this layer leads to a temperature inversion.

5. Altitude profile of temperature and total number density on Titan (Model)

6. Titan’s emission spectra in the ultraviolet

7. Composition of Titan’s atmosphere

8. Schematic of temperature profile on Titan

9. Photochemistry of Titan The minimum temperature at the tropopause is about 70 K. For many of the organic compounds found on Titan the measured abundance is above the saturated vapor pressure at the tropopause. The source of these species cannot therefore be the troposphere, but must be the stratosphere. Must be derived from volatile parent molecules. The absence of H 2 and the presence of abundant N 2 modify the chemistry considered previously for Jupiter and Saturn. On the planets radicals such as CH 3 or NH 2 derived from CH 4 and NH 3 react by abstraction of H from H 2 or by three body combination with H-atoms to return to the parent molecule. So-called ‘do nothing’ cycle

10. Photochemistry of Titan This cannot happen on Titan, so the less hydrogen-rich hydrocarbons are favored. Mixing ratios of C 2 H 6 are four times greater on Titan than on Saturn, those of C 2 H 2 are 27 times greater, and C 2 H 4, which cannot be detected on Saturn, is clearly detected on Titan. The key differences between Titan and the planets are the absence of back-reactions involving H and H2, the presence of processes involving N and N +, and the quenching of 1 CH 2 to 3 CH 2 by N 2 This leads to the formation of C 2 H 2, C 2 H 4 and C 3 H 4 from the triplet state.

11. Atmospheric chemistry on Titan

12. Photochemistry of Titan CH 4 + hν + N 2 → 3 CH 2 + H 2 (or 2H) + N 2 3 CH 2 + 3 CH 2 → C 2 H 4 +H 2 (or2H) Followed by: C 2 H 2 + hν → C 2 H + H C 2 H + CH 4 → C 2 H 2 + CH 3 These then lead to the formation of the other organic compounds 3 CH 2 + CH 4 → C 2 H 4 + H CH 3 + CH 3 + M → C 2 H 6 + M C 2 H + C 2 H 6 → C 2 H 2 + C 2 H 5 C 2 H 5 + CH 3 + M → C 3 H 8 + M

13. Theoretical altitude profiles of H2 and hydrocarbons on Titan

15. Altitude profiles of carbon species and H (Model)

16. Io

17. Very few, if any, impact craters on the surface. Surface is young Hundreds of volcanic calderas. Some are still active. Striking photographs have been taken from Voyager 1 of actual eruptions. Vapor from the vents of the volcanoes appears to be SO 2 or S. Optical emissions have been observed from atomic sulfur and oxygen Atmosphere is tenuous – pressure at surface about 10 -7 atmospheres.

18. Io, Sulfur saturation vapor pressure

19. Io Sulfur dioxide has a vapor pressure of 10 -9 bar in the polar regions (<98K) and on the night-side. But at the sub-solar point the pressure could be as high as 10 -7 bar, ~130K). Simplistic view of the atmosphere is a relatively dense atmosphere near the volcanoes and the sub-solar point, which becomes thin near the poles and on the dark side. Microwave observations show 4-35x10 -9 bar of SO 2 covering 3-18% of the surface – consistent with SO 2 being in equilibrium with the surface temperature. It has been suggested that O 2 at a pressure of 20x10 -9 also exists, but there is no direct evidence.

20. Io photochemistry Primary path for the dissociation of SO2 is as follows: SO 2 + hν(λ<221 nm) → SO + O SO 2 + hν(λ<221 nm) → S + O 2 Followed by: SO + SO → SO 2 + S S + O 2 → SO + O

21. SO 2 number density (N) and temperature (T) for Io (Model)

22. Distribution of major constituents on Io (Model)

23. Europa

24. Satellite of Jupiter Similar in composition to Io, but unlike Io has a thin outer layer of ice. Very few craters on Europa, suggesting a young and active surface. Images of Europa surface strongly resemble images of sea ice on Earth. Has a very tenuous atmosphere 10 -11 bar, composed of oxygen. Almost certainly not of biogenic origin. Most likely source is the bombardment of the icy surface by UV radiation, and charged particles in the solar wind. Has a weak magnetic field, which varies periodically as Europa moves through Jupiter’s massive magnetic field. Interpreted as signifying that Europa has a conducting layer beneath the surface – probably a salty ocean.

25. Callisto

26. The satellite of farthest from Jupiter. Surface is covered entirely with craters. Is very old. Callisto has the oldest and most cratered of any body yet discovered in the solar system (4 billion years). Has a very tenuous atmosphere composed of carbon dioxide. Has a weak magnetic field. Little evidence of tectonic activity