Michael Mendillo, Andrew Nagy, J. H. Waite Jr.'s Atmospheres in the Solar System: Comparative Aeronomy PDF

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By Michael Mendillo, Andrew Nagy, J. H. Waite Jr.

ISBN-10: 0875909892

ISBN-13: 9780875909899

ISBN-10: 1118669576

ISBN-13: 9781118669570

Published through the yankee Geophysical Union as a part of the Geophysical Monograph Series.

Atmospheres are an important elements of our universe. they're the single observable areas of stars and tremendous planets, either inside and past our sun approach. a few terrestrial-size our bodies (Venus, Earth, Mars, Titan and Triton) have everlasting atmospheres whereas others (e.g., Mercury, Moon, Io, and Europa) have tenuous gaseous envelopes that fluctuate day-by-day. Comets are tiny our bodies by means of planetary yardsticks, yet their atmospheres should be the most important noticeable items within the evening sky. Atmospheric technology strives to appreciate how the sort of varied set of atmospheres shape, evolve, and disappear.


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C o n t i n u i t y ) , energy, a n d m o m e n t u m . H e r e we o u t l i n e t h e m a i n c o m p o n e n t s of t h e s e e q u a t i o n s as t h e y r e l a t e t o t h e u p p e r a t m o s p h e r e s of t h e solar s y s t e m , r e v i e w i n g t h e salient r e s u l t s for p h o t o c h e m ­ istry, e n e r g e t i c s , a n d d y n a m i c s o n k e y t e r r e s t r i a l p l a n e t s , j o v i a n p l a n e t s , a n d satellites. 1. INTRODUCTION In this chapter we outline the background and recent results for the photochemistry, energetics, and winds in selected planetary and satellite upper atmospheres.

Unless otherwise stated, photolysis rates in s a t 1 AU are from Huebner et al [1992], a n d 2-body and 3-body r a t e coefficients (in c m s and c m s , respectively) are from Yung and DeMore [1999]. If t h e atmosphere of Mars were entirely C 0 , then relatively large abundances of C O and 0 would naturally arise in a 2:1 proportion, respectively, since t h e recombination reaction C O + 0 -»• C 0 is spin forbidden and so is very slow. 5 x 1 0 - ( 1 + 0 . 0 x i o 2 3 net: 3 2 3 2(S0 + H 0 x 2 2 2 2 0 0 / T Several other catalytic cycles exist, some involving t h e odd nitrogen families known as N O (made u p of N, N O , N 0 , N 0 , and 2 N 0 ) a n d N O (made up of NO* and H N 0 , H N 0 , and H 0 N 0 ) .

Gladstone, G. , M. Allen, and Y. L. Yung, Hydrocar­ bon photochemistry in the upper atmosphere of Jupiter, Icarus, 82, 1-52, 1996. -C. Gerard, and J. H. , A selfconsistent model of the jovian thermal structure, J. Geo­ phys. , 106, 12,933-12,952, 2001. Hinson, D. , Jupiter's ionosphere: results from the first Galileo radio occultation experiment, Geophys. Res. Lett, 24, 2107-2110, 1997. Hinson, D. , G. L. Tyler, J. L. Hollingsworth, and R. J. Wilson, Radio occultation measurements of forced atmo­ spheric waves on Mars, J.

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Atmospheres in the Solar System: Comparative Aeronomy by Michael Mendillo, Andrew Nagy, J. H. Waite Jr.

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