Были ли американцы на Луне? Опрос

Он сам не мог признаться ))

"И тебя вылечим".
Большой брат не любит громких слов, особенно разоблачений. )

угрожаешь?

Не. Напоминаю - предупреждение от роспотребсоюза о заклеивании микрофона и камеры на ноутбуке - получила?
Исполнила? )

Давным давно
Кстати, если мышке на брюшке заклеить лампочку обычным прозрачным скотчем, она перестает реагировать. Забавно получается

Проверим

Пробуй, только получится на оптической мышке ... или лазерной?

Он еще катает старый раритет с шариком. ))

The moon is older than previously believed
Date: July 29, 2019
Source: University of Cologne
Summary:
Fifty years after the first landing on the Moon, scientists have combined new geochemical information to determine the Moon's age using samples from different Apollo missions.

Early Moon formation inferred from hafnium–tungsten systematics
Maxwell M. Thiemens, Peter Sprung, Raúl O. C. Fonseca, Felipe P. Leitzke & Carsten Münker
Nature Geoscience (2019)

Abstract

The date of the Moon-forming impact places an important constraint on Earth’s origin. Lunar age estimates range from about 30 Myr to 200 Myr after Solar System formation. Central to this age debate is the greater abundance of 182W inferred for the silicate Moon than for the bulk silicate Earth. This compositional difference has been explained as a vestige of less late accretion to the Moon than to the Earth after core formation. Here we present high-precision trace element composition data from inductively coupled plasma mass spectrometry for a wide range of lunar samples. Our measurements show that the Hf/W ratio of the silicate Moon is higher than that of the bulk silicate Earth. By combining these data with experimentally derived partition coefficients, we found that the 182W excess in lunar samples can be explained by the decay of the now extinct 182Hf to 182W. 182Hf was only extant for the first 60 Myr after the Solar System formation. We conclude that the Moon formed early, approximately 50 Myr after the Solar System, and that the excess 182W of the silicate Moon is unrelated to late accretion.

Sample selection

Samples were provided by the Curation and Analysis Planning Team for Extraterrestrial Materials and selected to represent the major lithological units of the Moon as sampled by the NASA Apollo missions. To characterize their chemical composition, our particular focus lay on the quantification of any inherent U/W, Th/W and Hf/W variability as inferred from the few previous studies available. Some sample duplicity with previous studies allowed for an additional quality assessment. In total, lunar samples from Apollo 11 (three), Apollo 12 (six), Apollo 14 (three), Apollo 15 (six), Apollo 16 (four) and Apollo 17 (four) were analysed. Of these, seven were Apollo 11 or Apollo 17 high-Ti mare basalts and soils, 14 were low-Ti mare basalts from Apollo 12 and Apollo 15, two were Apollo 16 FANs, along with seven KREEP-rich samples, which included a meteorite and KREEP-rich breccias and KREEP basalts from the Apollo 14, 16 and 17 missions.

Все лунные образцы, привезенные Аполлонами потеряны, как нам тут говорят, а люди их во всю продолжают изучать (причем даже и не в США) и публикуют интересные научные статьи в лучших журналах... как же так?

Чёта возникают сомнения

Все лунные образцы, привезенные Аполлонами потеряны, как нам тут говорят, а люди их во всю продолжают изучать (причем даже и не в США) и публикуют интересные научные статьи в лучших журналах... как же так?

https://www.sciencedaily.com/releases/2019/07/190729111234.htm

https://www.nature.com/articles/s41561-019-0398-3

В обоих ссылках нет ни слова о том, что данные для этих статей получены самостоятельно. В них идет анализ тех данных, которые им предоставлены второй стороной, и делаются выводы из этого анализа. Кто является второй стороной? Угадайте с трех раз.
ЗЫ. Впрочем, и одного более чем достаточно.

Sample preparation

To obtain high-precision data, we measured all the elements of interest by isotope dilution and added several isotope tracers to ~100 mg (250 mg for anorthosites) of each sample prior to digestion. The mixed isotope tracers included 229Th–233U–236U and 183W–180Ta–180Hf–176Lu–94Zr mixed solutions. Samples were digested in 3 ml of double distilled HF and 3 ml of distilled HNO3 for 24 h at 120 °C. Prior to drydown, 0.5 ml of perchloric acid were added to ensure a sample-spike equilibrium for Th. Samples were redissolved with concentrated HNO3 and trace HF to ensure the redissolution of HFSE. These sample solutions were subsequently dried down again, and redissolved in 6 ml of 6 M HCl–0.06 M HF to ensure a full sample-spike equilibrium for HFSE. These samples were then aliquoted, with 10% of the solution used for conventional trace element analysis, 20% for W isotope dilution measurements and 70% for high-field-strength and U–Th element analysis. For a first batch of samples, an additional aliquot of 10% for U–Th was taken. The anorthosite samples were aliquoted with 85% for a combined HFSE, W and U–Th aliquot, and 15% for trace element analysis.

The trace element aliquot was dried down, dissolved in concentrated HNO3 and then dried down again. This residue was subsequently dissolved in 1 ml of concentrated HNO3, with 4 ml of MilliQ H2O added, and then diluted with MilliQ H2O to 50 ml. Conventional trace element analyses on these aliquots were performed at the Quadrupole ICP-MS laboratory at the Institut für Geowissenschaften at CAU zu Kiel using the procedure of Garbe-Schönberg51.

Our protocol to separate individual HFSE and U–Th cuts from lunar samples is a modified protocol based the literature22,52,53. During the protocol, individual cuts that contained a matrix, heavy rare earth elements (HREEs), Zr–Nb, Ta, Hf and U–Th were separated from the HFSE aliquot. Tungsten was separated from the W isotope dilution step via a separate set of anion-exchange resin microcolumns (Table 4 in Kleine et al.53).

In our HFSE protocol, the sample aliquots were dissolved in 3M HCl and loaded onto a Ln Spec resin column. Matrix and light REEs were eluted in 3 M HCl. An HREE fraction that contained the most Lu was eluted with 6M HCl, followed by elution of an HFSE cut that contained Ti–Zr–Nb–Hf–Ta–U–Th in 2M HF. A quantitative Zr/Nb aliquot was taken from this fraction52. The remaining HFSE cut was loaded onto a Bio-Rad column that contained an AG 1 × 8 100–200 mesh resin. The U–Th fraction was collected in 2M HF, and a Ti–Zr–Hf fraction was collected in 6M HNO3/0.2M HF. A clean Ta fraction was subsequently collected in 6M HNO3/0.2M HF/1% H2O2. The Ti–Zr–Hf fraction was dried down overnight and loaded onto the stage I Ln Spec resin column in 3M HCl. After clean-up in 6M HCl and MilliQ H2O, Ti was eluted using a 1M HNO3–2% H2O2 mixture54 and some Zr was eluted in 6M HCl−0.06M HF. Hafnium was finally eluted in 2M HF.

Separation of U–Th was performed in two ways, following a modified literature protocol55. For the first batch of samples, a full aliquot was used, whereas for the other batches the U–Th fraction from the 2M HF elution step above was taken. After drydown, the U- and Th-bearing cuts were dissolved in 1.5M HNO3, before being loaded onto columns that contained TRU-Spec resin (200–400 mesh). In a modification of the chemistry of Luo et al.55, all the major elements were initially eluted in 1.5M HNO3. After the removal of the rare earth elements in 3M HCl, Th was eluted in 0.2M HCl. Finally, U was eluted in 0.1M HCl/0.3M HF.

Given the low concentrations of the elements of interest in anorthosites, we performed a different separation protocol for these samples. About 70% of the 85% HFSE aliquots of anorthosites was loaded on an anion exchange resin in 1M HCl/0.5M HF solution. The eluted matrix cut and an additional fraction rinsed in 0.5M HCl/0.5M HF contained most of the Rb–Sr, Sm–Nd and U–Th. A fraction that contained Ti–Zr–Hf was collected in 6M HCl/0.06M HF, from which Hf was further purified using Ln Spec resin (see above). A W fraction was subsequently eluted in 6M HNO3/0.2M HF, followed by Ta elution in 6M HNO3/0.2M HF/1% H2O2. After drydown, the Ta cut was loaded again on the same anion resin column for clean-up, and the Ta was again eluted in 6M HNO3/0.2M HF/1% H2O2 after clean-up in 6M HNO3/0.2M HF. The remaining 15% of the anorthosite HFSE aliquots was loaded on Ln Spec resin in 3M HCl. Two fractions that contained HREE and Zr/Nb were eluted from the column in 6M HCl and 2M HF, as described above. The advantage of this approach is that a larger W fraction is collected, which thus avoids low sample-to-blank ratios during W isotope dilution measurements.

Прямо написано - МЫ измерили. И метод подготовки образцов описан и т.д.

https://www.nature.com/articles/s41561-019-0398-3

Это не они так сказали, а перевод такой. А про реальные измерения ими самими - ни слова.

Analytical protocols
All the isotope dilution measurements were performed using the Neptune MC-ICP-MS at the University of Cologne. Detailed descriptions of the analytical protocols for the HFSE measurements, analytical uncertainties and further references are given in Münker22. For 229Th/232Th measurements, we used a secondary electron multiplier ion counter equipped with an RPQ system on mass 229Th. The Th cuts were doped with the NBL CRM 112A U standard for a mass bias correction, and the ion counter was calibrated with concentration-matched IRM-035 and IRM 036 standards for ion counter yield corrections. For U measurements, mass bias was corrected using the measured 233U/236U of the spiked U cuts and the certified 233U/236U from Richter et al.56 for the doped IRM-3636 double spike used for preparation of the mixed U–Th tracer. Our external precision and accuracy for elemental ratios determined by isotope dilution that involved U and Th was typically better than ±1% for both U/W and Th/W (2σ relative standard deviation). Typical blanks used during the course of the measurements were below 50 pg for W, 66 pg for U, 32 pg for Th and 30 pg for Hf. These blanks proved negligible, with total a blank uncertainty, including propagated errors, of less than ±1%.

Results (and modelling constraints)
The measured HFSE and HFSE/U–Th ratios were distinct for different sample groups and mineralogy, with only small variations in U/W and Hf/W between samples from the same lithology. High-Ti basalts are particularly heterogeneous, with samples from the three measured localities that showed distinct Hf/W and U/W values. Apollo 17 high-Ti breccias both have similar values, with Hf/W ranging from 31 to 35, at a constant U/W of 1.9. This is distinct from Apollo 17 high-Ti mare basalts, for which U/W correlates positively with Hf/W. The Apollo 11 high-Ti mare basalts both have Hf/W of 42 and U/W of 2.2. Unique among all the samples are the Apollo 17 high-Ti mare basalts, which bear exceptionally high Hf/W ratios, between 120 and 150. Likewise, the low-Ti basalts plot as particularly distinctive groups according to the mission site. The Apollo 12 ilmenite basalts have a similar U/W to those of the Apollo 12 olivine and pigeonite basalts, of 2.07 and 2.25, respectively. However, they are distinct in their Hf/W, with both pigeonite-bearing basalts near 30 and ilmenite basalts of 43–48. The Apollo 15 quartz-normative and olivine-normative low-Ti basalts have different U/W, ranging from an average of 2.45 in the former to 1.75 in the latter. The Hf/W ratios of the two low-Ti basalt groups also vary from 45 (quartz-normative) to 30 (olivine normative). Whereas the olivine-normative low-Ti basalts of both Apollo 15 and Apollo 12 have identical Hf/W, their U/W differ significantly, from among the lowest values (1.63) measured to the highest (2.53), respectively. The KREEP-rich samples have a very narrow range in Hf/W of ~20. The U/W of KREEP samples has the largest spread, with most samples in the range 1.63 to 2.51, and minimum and maximum values of 0.54 and 3.38, respectively.

Ну, вот судьба нескольких граммов известна. Осталось еще 300 с лихвой килограмм.
Кстати, по той ссылке самой статьи я так и не нашел. И твоей цитаты тоже . Или она под платными кнопками?

Да, он мне в личке писал, что амеров не было на Луне, просто он придуривается на форуме, шутит так

Чёта возникают сомнения, в твоём высшем образовании, коли ты пишешь "ВОВСЮ" - раздельно...