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31.
Otto Pratje 《International Journal of Earth Sciences》1942,33(1):8-15
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33.
Otto Wilckens 《International Journal of Earth Sciences》1926,17(3):233-239
Ohne Zusammenfassung 相似文献
34.
Otto Wilckens 《International Journal of Earth Sciences》1943,34(2-6):278-279
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35.
Salomon Wilheim Salomon Cloos Steinmann Otto Wilckens Donath E. Spengler Jurasky Wilckens 《International Journal of Earth Sciences》1928,19(2):146-153
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Reviewing the existing studies of public perception and drawing analogies from other risk technologies, this paper explores the public positions on research and implementation of geoengineering as a means to combat climate change. Existing studies on geoengineering perceptions show low levels of awareness and a lack of knowledge. Hence, existing attitudes on geoengineering can be judged instable and stimulus-dependent. When judged in isolation, at least one third favors the use of geoengineering technologies preferring CDR over SRM technologies; when judged in comparison to other climate mitigation options, approval rates lose considerably support. Moreover, people seem to cautiously support research but oppose deployment while attitude formation depends on personal values and belief systems. The results of the empirical studies were fed into a Delphi workshop with experts for reflecting on the future development of public opinion and for designing a communication and public involvement process that corresponds to the empirical insights gained from the perception studies. 相似文献
38.
Robert Connon Smith Otto Mehes Dave Vande Putte Nigel A. Hawkins 《Monthly notices of the Royal Astronomical Society》2005,360(1):364-374
Simultaneous spectroscopic and photometric observations of the Z Cam type dwarf nova SY Cancri were used to obtain absolute flux calibrations. A comparison of the photometric calibration with a wide-slit spectrophotometric calibration showed that either method is equally satisfactory. A radial velocity study of the secondary star, made using the far-red Na i doublet, yielded a semi-amplitude of K 2 = 127 ± 23 km s−1 . Taking the published value of 86 ± 9 km s−1 for K 1 gives a mass ratio of q = M 2 / M 1 = 0.68 ± 0.14 ; this is very different from the value of 1.13 ± 0.35 quoted in the literature. Using the new lower mass ratio, and constraining the mass of the white dwarf to be within reasonable limits, then leads to a mass for the secondary star that is substantially less than would be expected for its orbital period if it satisfied a main-sequence mass–radius relationship. We find a spectral type of M0 that is consistent with that expected for a main-sequence star of the low mass we have found. However, in order to fill its Roche lobe, the secondary must be significantly larger than a main-sequence star of that mass and spectral type. The secondary is definitely not a normal main-sequence star. 相似文献
39.
Alan E. RUBIN Paul BENOIT Blaine REED Otto EUGSTER Ernst POLNAU 《Meteoritics & planetary science》1996,31(6):925-927
Abstract— Richfield is a moderately shocked (shock stage S4) LL3.7 genomict breccia find consisting mainly of light-colored recrystallized clasts and dark clasts exhibiting significant silicate darkening; a few impact-melt-rock clasts and LL5 chondrite clasts also occur. The cosmic-ray exposure age of 14.5 Ma is indistinguishable from the main exposure peak for LL chondrites (15 Ma). Although the exposure ages indicate little He loss, the gas-retention ages indicate high gas losses that must have occurred prior to or during ejection from the LL parent body. 相似文献
40.
Otto Wilckens 《International Journal of Earth Sciences》1925,16(2):128-142
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