Perceptive of the pyroxene-bearing micrometeorites and their relation to chondrites          下载免费PDF全文

N. G. Rudraswami  D. Fernandes  Agnelo De Araujo  M. Shyam Prasad  S. Taylor 《Meteoritics & planetary science》2018,53(10):2035-2050

We studied 149 pyroxenes from 69 pyroxene-bearing micrometeorites collected from deep-sea sediments of the Indian Ocean and South Pole Water Well at Antarctica, Amundsen-Scott South Pole station. The minor elements in pyroxenes from micrometeorites are present in the ranges as follows: MnO ~0.0–0.4 wt%, Al₂O₃ ~0.0–1.5 wt%, CaO ~0.0–1.0 wt%, Cr₂O₃ ~0.3–0.9 wt%, and FeO ~0.5–4 wt%. Their chemical compositions suggest that pyroxene-bearing micrometeorites are mostly related to precursors from carbonaceous chondrites rather than ordinary chondrites. The Fe/(Fe+Mg) ratio of the pyroxenes and olivines in micrometeorites shows similarities to carbonaceous chondrites with values lying between 0 and 0.2, and those with values beyond this range are dominated by ordinary chondrites. Atmospheric entry of the pyroxene-bearing micrometeorites is expected to have a relatively low entry velocity of <16 km s⁻¹ and high zenith angle (70–90°) to preserve their chemical compositions. In addition, similarities in the pyroxene and olivine mineralogical compositions between carbonaceous chondrites and cometary particles suggest that dust in the solar system is populated by materials from different sources that are chemically similar to each other. Our results on pyroxene chemical compositions reveal significant differences with those from ordinary chondrites. The narrow range in olivine and pyroxene chemical compositions are similar to those from carbonaceous chondrites, and a small proportion to ordinary chondrites indicates that dust is largely sourced from carbonaceous chondrite-type bodies.  相似文献   

Study of Lateral Sedimentation in the Western Atlantic on Cruise 53 of the R/V Akademik Ioffe     

Ivanova  E. V.  Murdmaa  I. O.  Borisov  D. G.  Ovsepyan  E. A.  Simagin  N. V.  Mutovkin  A. D.  Nemchenko  N. V.  Kornilova  M. O.  Sud’in  V. V.  Novikov  Yu. V. 《Oceanology》2018,58(6):932-934

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On Increasing the Accuracy of Star Trackers to Subsecond Levels     

A. I. Zacharov  N. L. Krusanova  I. V. Moskatiniev  M. E. Prohorov  O. Y. Stekol’shchikov  V. K. Sysoev  M. S. Tuchin  A. D. Yudin 《Solar System Research》2018,52(7):636-643

Modern star trackers are based on photodetector arrays such as CCD or CMOS arrays. The accuracy of commercially available devices is ~1–3 arcseconds. However, the development of the space industry calls for higher orientation accuracies, which are needed in laser space communications, monitoring of near-Earth space and space debris, high-precision global mapping, and remote sensing of the Earth. The problems associated with enhancing the accuracy of modern star trackers are discussed.  相似文献   

Surface Oscillations of a Free-Falling Droplet of an Ideal Fluid     

A. V. Kistovich  Yu. D. Chashechkin 《Izvestiya Atmospheric and Oceanic Physics》2018,54(2):182-188

According to observations, drops freely falling in the air under the action of gravity are deformed and oscillate in a wide range of frequencies and scales. A technique for calculating surface axisymmetric oscillations of a deformed droplet in the linear approximation under the assumption that the amplitude and wavelength are small when compared to the droplet diameter is proposed. The basic form of an axisymmetric droplet is chosen from observations. The calculation results for surface oscillations agree with recorded data on the varying shape of water droplets falling in the air.  相似文献   

Monitoring Anthropogenic Impact on Some Coastal Water Areas of the Black Sea Using Multispectral Satellite Imagery     

Bondur  V. G.  Vorobyev  V. E.  Zamshin  V. V.  Serebryany  A. N.  Latushkin  A. A.  Li  M. E.  Martynov  O. V.  Hurchak  A. P.  Grinchenko  D. V. 《Izvestiya Atmospheric and Oceanic Physics》2018,54(9):1008-1022

Izvestiya, Atmospheric and Oceanic Physics - The results of comprehensive monitoring of anthropogenic impact on some coastal water areas of the Black Sea are presented. Multispectral satellite...  相似文献   

Subphotospheric Resonator and Local Oscillations in Sunspots     

Yu. D. Zhugzhda 《Astronomy Letters》2018,44(5):331-336

The conditions under which the subphotospheric slow-wave resonator can be responsible for the local oscillations in a sunspot have been determined. A rich spectrum of local 3-min oscillations can be produced by the subphotospheric resonator only if the magnetic field in the resonator magnetic flux tube is much weaker than the surrounding sunspot magnetic field. Convective upflows of hot plasma in the sunspot magnetic field satisfy this condition. Consequently, there must be a correlation between the local oscillations and umbral dots, because the latter are produced by convective flows. Various modes of operation of the subphotospheric resonator give rise to wave packets of 3-min oscillations and umbral flashes. It is shown that giant local umbral flashes can emerge under certain conditions for the excitation of oscillations in the subphotospheric resonator.  相似文献   

Results of Photometric and Spectroscopic Observations of the Young Variable Star V730 Cep     

V. P. Grinin  K. A. Antonyuk  I. S. Potravnov  D. Mkrtichian 《Astronomy Letters》2018,44(12):798-802

We present the results of our photometric (V RI) and spectroscopic observations of the young variable star V730 Cep (MisV1147) classified by Uemura et al. (2004) as a Herbig Be star. Our photometry confirms the conclusion of the above authors that this star has a complex pattern of variability including periodic or quasi-periodic brightness variations with a period of about 14 days and deep Algol-like minima typical for UX Ori stars. Our spectroscopy shows that the classification of V730 Cep as a Herbig Be star is wrong. Actually, this star has a much lower temperature and belongs to the family of T Tauri stars. This allows us to explain the nature of the unusual photometric activity of V730 Cep based on a combination of two well-known models of variable circumstellar extinction applied to young stars: AA Tau- and UX Oritype variability. It follows from our observations that the color tracks on the V ?(V ?I) color–magnitude diagram for these models slightly differ: the AA Tau-type variability of circumstellar extinction is caused by larger grains than the UX Ori-type variability. Such a difference can be due to an increase in the characteristic sizes of circumstellar dust as the star is approached and has a simple explanation: small dust grains evaporate faster than large ones.  相似文献   

西北太平洋深海海山的一种蛇尾新记录     

张东声  鹿博  王春生  蒂莫西&#;奥哈拉 《海洋学报(英文版)》2018,37(10):180-184

Ophioleila elegans是一种非常少见的蛇尾。2014年大洋35航次中利用“蛟龙”号载人潜器在西北太平洋麦哲伦海山链的采薇平定海山水深1660m处采集到2株该种标本。该种首次发现于夏威夷海山相似的生境当中，本次采集到的样品是继首次发现之后的再次公开报道。本文中对该种的形态学特征，如腕部骨骼等，进行了更加详细的研究，同时基于COI序列进行系统发育分析。形态和系统发育分析的结果都表明，Ophioleila属与辐蛇尾科更加接近。  相似文献   

Stars with Discrepant <Emphasis Type="Italic">v</Emphasis> sin <Emphasis Type="Italic">i</Emphasis> as Derived from the Ca II 3933 and Mg II 4481 Å Lines. VII. HD9531 (SB), HD31592 (SB2), HD129174 (SB?)     

J. Zverko  I. Iliev  I. I. Romanyuk  I. Stateva  D. O. Kudryavtsev  E. A. Semenko 《Astrophysical Bulletin》2018,73(3):351-362

In this paper of the series we analyze three stars listed among stars with discrepant v sin i: HD9531 and HD31592, which also show radial velocity variations inherent to spectroscopic binaries, and HD129174 which is an Mn-type star with a possible magnetic field. In HD9531 we confirm the radial velocity derived fromthe hydrogen lines as well as fromthe Ca II line at 3933 Å as variable. The profile of the calcium line also appears variable, and with the estimated magnetic induction B_e = ?630 ± 1340 G, this suggests that the abundance of calcium possibly varies over the surface of the star. We identified the lines of the secondary component in the spectrum of HD31592 revealing thus it is an SB2 binary with B9.5V and A0V components. While the primary star rotates with v sin i = 50 km s^?1, the secondary star is faster with v sin i = 170 km s^?1. We find that only 60% of the Mn lines identified in the spectrum of HD129174 can be fitted with a unique abundance value, whereas the remaining lines are stronger or fainter. We also identified two Xe II lines at 5339.33 Å and 5419.15 Å and estimated their log g f.  相似文献   

<Emphasis Type="Italic">Wind</Emphasis> Magnetic Clouds for the Period 2013 – 2015: Model Fitting,Types, Associated Shock Waves,and Comparisons to Other Periods     

R. P. Lepping  C.-C. Wu  D. B. Berdichevsky  A. Szabo 《Solar physics》2018,293(4):65

We give the results of parameter fitting of the magnetic clouds (MCs) observed by the Wind spacecraft for the three-year period 2013 to the end of 2015 (called the “Present” period) using the MC model of Lepping, Jones, and Burlaga (J. Geophys. Res.95, 11957, 1990). The Present period is almost coincident with the solar maximum of the sunspot number, which has a broad peak starting in about 2012 and extending to almost 2015. There were 49 MCs identified in the Present period. The modeling gives MC quantities such as size, axial attitude, field handedness, axial magnetic-field strength, center time, and closest-approach vector. Derived quantities are also estimated, such as axial magnetic flux, axial current density, and total axial current. Quality estimates are assigned representing excellent, fair/good, and poor. We provide error estimates on the specific fit parameters for the individual MCs, where the poor cases are excluded. Model-fitting results that are based on the Present period are compared to the results of the full Wind mission from 1995 to the end of 2015 (Long-term period), and compared to the results of two other recent studies that encompassed the periods 2007?–?2009 and 2010?–?2012, inclusive. We see that during the Present period, the MCs are, on average, slightly slower, slightly weaker in axial magnetic field (by 8.7%), and larger in diameter (by 6.5%) than those in the Long-term period. However, in most respects, the MCs in the Present period are significantly closer in characteristics to those of the Long-term period than to those of the two recent three-year periods. However, the rate of occurrence of MCs for the Long-term period is \(10.3~\mbox{year}^{-1}\), whereas this rate for the Present period is \(16.3~\mbox{year}^{-1}\), similar to that of the period 2010?–?2012. Hence, the MC occurrence rate has increased appreciably in the last six years. MC Type (N–S, S–N, All N, All S, etc.) is assigned to each MC; there is an inordinately large percentage of All S, by about a factor of two compared to that of the Long-term period, indicating many strongly tipped MCs. In 2005, there was a distinct change in variability and average value (viewed at \(1/2\) year averages) of the duration, MC speed, axial magnetic field strength, axial magnetic flux, and total current to lower values. In the Present period, upstream shocks occur for 43% of the 49 cases; for comparison, the Long-term rate is 56%.  相似文献