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The loss of ions from Venus through the plasma wake 总被引:1,自引:0,他引:1
Barabash S Fedorov A Sauvaud JJ Lundin R Russell CT Futaana Y Zhang TL Andersson H Brinkfeldt K Grigoriev A Holmström M Yamauchi M Asamura K Baumjohann W Lammer H Coates AJ Kataria DO Linder DR Curtis CC Hsieh KC Sandel BR Grande M Gunell H Koskinen HE Kallio E Riihelä P Säles T Schmidt W Kozyra J Krupp N Fränz M Woch J Luhmann J McKenna-Lawlor S Mazelle C Thocaven JJ Orsini S Cerulli-Irelli R Mura M Milillo M Maggi M Roelof E Brandt P Szego K Winningham JD Frahm RA Scherrer J Sharber JR Wurz P 《Nature》2007,450(7170):650-653
Venus, unlike Earth, is an extremely dry planet although both began with similar masses, distances from the Sun, and presumably water inventories. The high deuterium-to-hydrogen ratio in the venusian atmosphere relative to Earth's also indicates that the atmosphere has undergone significantly different evolution over the age of the Solar System. Present-day thermal escape is low for all atmospheric species. However, hydrogen can escape by means of collisions with hot atoms from ionospheric photochemistry, and although the bulk of O and O2 are gravitationally bound, heavy ions have been observed to escape through interaction with the solar wind. Nevertheless, their relative rates of escape, spatial distribution, and composition could not be determined from these previous measurements. Here we report Venus Express measurements showing that the dominant escaping ions are O+, He+ and H+. The escaping ions leave Venus through the plasma sheet (a central portion of the plasma wake) and in a boundary layer of the induced magnetosphere. The escape rate ratios are Q(H+)/Q(O+) = 1.9; Q(He+)/Q(O+) = 0.07. The first of these implies that the escape of H+ and O+, together with the estimated escape of neutral hydrogen and oxygen, currently takes place near the stoichometric ratio corresponding to water. 相似文献
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Discovery of an aurora on Mars 总被引:1,自引:0,他引:1
Bertaux JL Leblanc F Witasse O Quemerais E Lilensten J Stern SA Sandel B Korablev O 《Nature》2005,435(7043):790-794
In the high-latitude regions of Earth, aurorae are the often-spectacular visual manifestation of the interaction between electrically charged particles (electrons, protons or ions) with the neutral upper atmosphere, as they precipitate along magnetic field lines. More generally, auroral emissions in planetary atmospheres "are those that result from the impact of particles other than photoelectrons" (ref. 1). Auroral activity has been found on all four giant planets possessing a magnetic field (Jupiter, Saturn, Uranus and Neptune), as well as on Venus, which has no magnetic field. On the nightside of Venus, atomic O emissions at 130.4 nm and 135.6 nm appear in bright patches of varying sizes and intensities, which are believed to be produced by electrons with energy <300 eV (ref. 7). Here we report the discovery of an aurora in the martian atmosphere, using the ultraviolet spectrometer SPICAM on board Mars Express. It corresponds to a distinct type of aurora not seen before in the Solar System: it is unlike aurorae at Earth and the giant planets, which lie at the foot of the intrinsic magnetic field lines near the magnetic poles, and unlike venusian auroras, which are diffuse, sometimes spreading over the entire disk. Instead, the martian aurora is a highly concentrated and localized emission controlled by magnetic field anomalies in the martian crust. 相似文献
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