Titlebook: Giant Planets of Our Solar System; Atmospheres, Composi Patrick G. J. Irwin Book 2009Latest edition Springer-Verlag Berlin Heidelberg 2009

頌揚(yáng)本人

Silent-Ischemia

Formation of the giant planets,ng”. As the universe expanded and cooled, numerous particle physics processes and particle-antiparticle annihilations occurred (e.g., Krane, 1996). After about . = 6 s, the universe consisted of some number . protons, . electrons, 0.16. neutrons, 10.. photons, and 10.. neutrinos, all at a temperatur

vasospasm

Evolution processes in outer planet atmospheres,er or lesser extent) evolved over time through the action of a number of possible processes including thermal escape, cometary bombardment, and internal differentiation. In this chapter we will outline the principal evolution mechanisms and estimate their effects on the present-day composition of th

小丑

Vertical structure of temperature, composition, and clouds,. Remote-sounding and . observations of the vertical profiles of pressure, temperature, and composition provide constraints on vertical motion, mixing, heat sources, deep composition, and photochemistry. These observations are complemented by observations of vertical cloud structure.

Flatter

Dynamical processes,scussed transport mechanisms such as convection and eddy mixing. Of course the real atmospheres of planets are three-dimensional and thus to understand fully the observations of ground-based telescopes and spacecraft missions, we need to understand how planetary atmospheres move and how heat and mat

hereditary

Radiative transfer processes in outer planetary atmospheres,are available were made from the . entry probe, which sampled a single, probably not very representative, region of the planet, namely a 5 μm hotspot. Hence, the bulk of our knowledge of the composition, cloud structure, and dynamics of these planets has not come from direct measurements, but instea

泄露

Sources of remotely sensed data on the giant planets,sorption features of different gases (and theoretically aerosols) are visible in these spectra. Clearly much can be learned about the atmospheres from observing the spectra of these planets, and in this chapter we will review the measurements that have been made to date and how they may be used.

Cupidity

IRATE

https://doi.org/10.1007/978-3-540-85158-5AAS; AGU; Cloud; DPS; EGU; giant planets; planetary atmospheres; solar system; temperature

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