Titlebook: Comparative Planetology with an Earth Perspective; Proceedings of the F Moustafa T. Chahine,Michael F. A’Hearn,Neil L. Nic Conference proce

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書(shū)目名稱Comparative Planetology with an Earth Perspective影響因子(影響力)




書(shū)目名稱Comparative Planetology with an Earth Perspective影響因子(影響力)學(xué)科排名




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書(shū)目名稱Comparative Planetology with an Earth Perspective讀者反饋學(xué)科排名

MOCK

Geology of Terrestrial Planets with Dynamic Atmospheres,m) and exogenic processes (impact cratering and gradation). The present appearance of planetary surfaces is the result of the complex interplay of these processes and is linked to the evolution of planets and their environments. Terrestrial planets that have dynamic atmospheres are Earth, Mars, and

Monotonous

Constraints on the Martian Cratering Rate Based on the SNC Meteorites and Implications for Mars Clismic ray exposure ages and number of impacts as a constraint on absolute rates. The crystallization ages of the SNC meteorites appear to constrain the Martian cratering rate to be 4xLunar or more if the parent lavas are in the north of Mars and the number of SNC ejecting impacts are small. If the SN

任命

Factors Controlling Volcanism and Tectonism in Solar System Solid Bodies,nd Mikhail A. Kreslaysky, Kharkov Astronomical Observatory, Kharkov, Ukraine, to look for fundamental laws which control the formation and evolution of the solar system solid bodies. This work was published in a Russian journal [1], and thus is almost unknown abroad, although it has been translated

probate

Giant Planet Formation,wn only in stars. The condensible element cores of the gas-giants grow by solid body accretion while envelope formation is governed by ‘stellar-like’ equilibria and the dynamic departures thereof. Two hypotheses for forming Uranus/Neptune-type planets — at sufficiently large heliocentric distances w

雜役

雜役

Origin of the Major Planet Atmospheres: Clues from Trace Species,ne, resulted from two sources: outgassing from planetary interiors during the accretionary heating phase — the planetesimals making up the core were composed of grains, ices and possibly clathrates — and direct capture of gases from the solar nebula. It is not apparent, however, whether the present

BIAS

The Chemical Atmospheric Composition of the Giant Planets,the primordial nebula from which they formed. However, this image has strongly evolved over the past twenty years, due to new developments of ground-based infrared spectroscopy, coupled with the success of the Voyager space mission..Significant differences were measured in the abundances of helium,

善辯

NH3, H2S, and the Radio Brightness Temperature Spectra of the Giant Planets,s comparison reveals evidence for fundamental differences in the compositions of Uranus’ and Neptune’s upper tropospheres, particularly in their ammonia (NH.) and hydrogen sulfide (H.S) mixing ratios, despite those planets’ outward similarities. The tropospheric abundances of these constituents yiel

舊式步槍

Cryovolcanism on the Icy Satellites,to many silicate volcanic terrains, including what appear to be volcanic rifts, calderas and solidified lava lakes, flow fields, breached cinder cones or stratovolcanoes, viscous lava domes, and sinuous rilles. Most other satellites have terrains that are different in the important respect that no o