Wing-huen Ip, Wing-huen Ip, Yun-Tai Chen's Advances in Geosciences: Planetary Science, Vol. 7 PDF

By Wing-huen Ip, Wing-huen Ip, Yun-Tai Chen

ISBN-10: 9812709886

ISBN-13: 9789812709882

Advances in Geosciences is the results of a concerted attempt in bringing the most recent effects and making plans actions on the topic of earth and area technological know-how in Asia and the overseas area. the quantity editors are all best scientists of their learn fields overlaying six sections: Hydrological technology (HS), Planetary technology (PS), sunlight Terrestrial (ST), stable Earth (SE), Ocean technological know-how (OS) and Atmospheric technology (AS). the most function is to focus on the medical matters necessary to the research of earthquakes, tsunamis, atmospheric airborne dirt and dust storms, weather switch, drought, flood, typhoons, monsoons, area climate, and planetary exploration.

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Submillimeter wave astronomy satellite observations of the Martian atmosphere: temperature and vertical distribution of water vapor, Astrophys. J. 539 (2000) L143. 4. M. A. Gurwell, E. A. Bergin, G. J. Melnick and V. Tolls, Mars surface and atmospheric temperature during the 2001 global dust storm, Icarus 175 (2005) 23. 5. R. T. Clancy, B. J. Sandor, G. H. Moriarty-Schieven and M. D. Smith, Mesoscale winds and temperatures from JCMT sub-millimeter CO line observations during the 2003 and 2005 Mars oppositions, Abstract of “Second Workshop on Mars Atmosphere Modelling and Observations”, Granada, Spain (2006), pp.

O. A. Gusev and A. A. Kutepov, Non-LTE gas in planetary atmospheres, in Stellar Atmosphere Modeling, eds. I. Hubeny, D. Mihalas and K. Werner, ASP Conf. Ser. 288 (2003) 318. 13. T. Nakajima and M. Tanaka, Matrix formulations for the transfer of solar radiation in a plane-parallel scattering atmosphere, J. Quant. Spectrosc. Radiat. Transfer 35 (1986) 13. 14. F. Forget, F. Hourdin, R. Fournier, C. Hourdin, O. Talagrand, M. Collins, S. R. Lewis, P. L. -P. Huot, Improved general circulation models of the Martian atmosphere from the surface to above 80 km, J.

The wind velocity was directly measured from Doppler shifts of CO lines. We emphasize that these wind data obtained from the microwave measurements are unique for the Martian atmosphere. The descending landers (Viking and Mars Pathfinder) performed the only other available wind measurements. The simulated temperature in the Martian mesosphere is considerably higher than shown by the JCMT microwave data. However, the model temperature at 60–70 km is ∼10 K lower in summer solstice than in spring and autumn equinoxes, which is consistent with the measurements.

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Advances in Geosciences: Planetary Science, Vol. 7 by Wing-huen Ip, Wing-huen Ip, Yun-Tai Chen

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