Giant Planets of Our Solar System: An Introduction by Patrick Irwin

By Patrick Irwin

This bookreviews the present kingdom of data of the atmospheres of the large gaseous planets: Jupiter, Saturn, Uranus, and Neptune. the present theories in their formation are reviewed and their lately saw temperature, composition and cloud buildings are contrasted and in comparison with basic thermodynamic, radiative move and dynamical versions. The tools and methods which were used to remotely degree their atmospheric homes also are reviewed, and the most likely improvement of outer planet observations over the subsequent twenty years is printed.

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3 (McCaughrean et al. 1994). These polar jets are probably collimated both by the dense circumstellar disc itself and by the magnetic ®eld of the protostars. They are seen to be episodic in nature, which is consistent with them being fed by turbulent infall of the inner circumstellar disc. However, while this bipolar out¯ow would have carried off as much as 10% of the nebula mass, it would not have accounted for much of the angular momentum. (2) T-tauri phase. The Sun is currently about half way though its main sequence (Lewis, 1995).

J. Lissauer (2001) Planetary Sciences. Cambridge University Press, Cambridge, UK. -P. Bibring, and M. Blanc (1995) The Solar System (2nd Edition). Springer, Berlin. Jones, B. W. (1999) Discovering the Solar System. John Wiley & Sons, Chichester, UK. Miner, E. D. (2000) Uranus: The planet, rings and satellites (2nd Edition). Springer±Praxis, Chichester, UK. Miner, E. D. and R. R. Wessen (2002) Neptune: The Planet, Rings and Satellites. Springer±Praxis, Chichester, UK. Rogers, J. H. (1995) The Giant Planet Jupiter.

In the outer disc, beyond perhaps 50 AU the nebula density is predicted to have been so low that turbulence would not have been able to play such an important role. In this low-turbulence region, material would rotate about 26 Formation of the giant planets [Ch. 122 mm) image of HH212. 5-m telescope in Spain. The image shows the bi-polar jet from the formation of a star near the centre of the frame and hence the circumstellar disc appears to be almost edge-on. Material can be seen to be ejected in pulses and there is a clear symmetry between the pulses in the upper and lower jets.

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