Sounding Rocket Observations of Active Region Soft X-Ray Spectra Between 0.5 and 2.5 nm Using a Modified SDO/EVE Instrument     

Seth Wieman  Leonid Didkovsky  Thomas Woods  Andrew Jones  Christopher Moore 《Solar physics》2016,291(12):3567-3582

Spectrally resolved measurements of individual solar active regions (ARs) in the soft X-ray (SXR) range are important for studying dynamic processes in the solar corona and their associated effects on the Earth’s upper atmosphere. They are also a means of evaluating atomic data and elemental abundances used in physics-based solar spectral models. However, very few such measurements are available. We present spectral measurements of two individual ARs in the 0.5 to 2.5 nm range obtained on the NASA 36.290 sounding rocket flight of 21 October 2013 (at about 18:30 UT) using the Solar Aspect Monitor (SAM), a channel of the Extreme Ultaviolet Variability Experiment (EVE) payload designed for underflight calibrations of the orbital EVE on the Solar Dynamics Observatory (SDO). The EVE rocket instrument is a duplicate of the EVE on SDO, except the SAM channel on the rocket version was modified in 2012 to include a freestanding transmission grating to provide spectrally resolved images of the solar disk with the best signal to noise ratio for the brightest features, such as ARs. Calibrations of the EVE sounding rocket instrument at the National Institute of Standards and Technology Synchrotron Ultraviolet Radiation Facility (NIST/SURF) have provided a measurement of the SAM absolute spectral response function and a mapping of wavelength separation in the grating diffraction pattern. We discuss techniques (incorporating the NIST/SURF data) for determining SXR spectra from the dispersed AR images as well as the resulting spectra for NOAA ARs 11877 and 11875 observed on the 2013 rocket flight. In comparisons with physics-based spectral models using the CHIANTI v8 atomic database we find that both AR spectra are in good agreement with isothermal spectra (4 MK), as well as spectra based on an AR differential emission measure (DEM) included with the CHIANTI distribution, with the exception of the relative intensities of strong Fe?xvii lines associated with \(2p^{6}\)–\(2p^{5}3{s}\) and \(2p^{6}\)–\(2p^{5}3{d}\) transitions at about 1.7 nm and 1.5 nm, respectively. The ratio of the Fe?xvii lines suggests that the AR 11877 is hotter than the AR 11875. This result is confirmed with analysis of the active regions imaged by X-ray Telescope (XRT) onboard Hinode.  相似文献   

滇东北麻栗坪铅锌矿床微量元素分布与赋存状态:LA-ICPMS研究   总被引：4，自引：2，他引：2  

胡宇思  叶霖  黄智龙  李珍立  韦晨  Danyushevskiy Leonid 《岩石学报》2019,35(11):3477-3492

位于扬子板块西南缘的"川滇黔接壤铅锌矿集区"是我国西南大面积低温成矿域的重要组成部分,麻栗坪铅锌矿床位于该矿集区昭通-曲靖成矿带中段,是近年来滇东北地区新发现的铅锌矿床。本文以麻栗坪铅锌矿不同硫化物为研究对象,通过LA-ICPMS原位点测试和元素Mapping分析,尝试揭示该矿床中Ge、Cd和In等微量元素在不同硫化物中分布规律与赋存状态。本次研究发现,麻栗坪矿床不同硫化物中富集的微量元素明显不同,闪锌矿主要富集Mn、Cu、Sn、Cd、In和Ge,而方铅矿主要富集Ag、Sb和Se,黄铁矿则富集As、Co和Ni。闪锌矿是分散元素Ge、In和Cd的主要载体矿物,且Cd、Ge、In、Mn、As、Sb和Ag以类质同象形式赋存于闪锌矿中;而Cu则主要以类质同象形式存在,部分Cu以黄铜矿的显微包裹体形式赋存于闪锌矿中,其中以类质同象赋存于闪锌矿中Cu和Ge呈现明显的相关性,可能暗示其与Zn的置换方式为:3Zn2+Ge4++2Cu+。总体上,该矿床闪锌矿以富集Cd、Ge,贫Fe、Mn、Co、Sn为特征,这些微量元素组成与典型MVT型矿床基本一致,明显有别于喷流沉积和岩浆热液型矿床,而与中低温条件下形成的闪锌矿微量元素组成相似。结合该矿床后生成矿特征明显等地质地球化学研究成果,我们认为该矿床应属于MVT型铅锌矿床。值得注意的是,该矿床闪锌矿相对富集In,可能暗示其形成具有特殊性,这可能与其成矿流体在长距离运移过程中所流经地层有关,该类流体活化萃取了基底地层的中-酸性岩浆岩或火山碎屑岩中的In,致使矿床中闪锌矿相对富集In。  相似文献   

Simultaneous volume measurements of post-perovskite and perovskite in MgSiO3 and their thermal equations of state     

Tetsuya Komabayashi  Kei Hirose  Emiko Sugimura  Nagayoshi Sata  Yasuo Ohishi  Leonid S. Dubrovinsky 《Earth and Planetary Science Letters》2008,265(3-4):515-524

Simultaneous volume measurements of MgSiO₃ post-perovskite (PPv) and perovskite (Pv) were performed in a diamond anvil cell (DAC) combined with synchrotron X-rays. An externally-heated DAC was used in addition to a laser-heated DAC for the volume measurement experiment at high temperatures. The volume data were collected in the stability field of post-perovskite from 115 to 130 GPa. The temperature generated in the externally-heated and the laser-heated DACs for the volume measurement were up to 832 and 2330 K, respectively. Using two different but complementary heating techniques, we collected the data at a wide temperature range from 300 to 2330 K. The obtained P-V-T data for PPv and Pv were fitted to a third-ordered Birch-Murnaghan equation of state (EOS). For a precise comparison of the volume between the two phases, the EOSs were constructed based on the same pressure scale of MgO. The simultaneous volume measurements and the volumes calculated from the determined EOSs demonstrate that the volume difference between PPv and Pv of about 1.5% is almost constant with increasing temperature to 4000 K at the transition. At the base of the mantle, this density difference corresponds to a temperature anomaly of 1300 K without the phase transition due to the very small thermal expansivity of minerals, which has a significant effect on mantle dynamics. The thermal expansivity contrast between the top and the bottom of the mantle is a factor of 3.6. From a mantle convection study, this value suggests that huge and hot plumes are formed at the core–mantle boundary.  相似文献   

Magneto-ionospheric effects of the solar eclipse of March 20, 2015, over Kharkov     

L.?F.?ChernogorEmail author  K.?P.?Garmash 《Geomagnetism and Aeronomy》2017,57(1):72-83

The results of observations of disturbances in the lower and middle ionosphere and in the geomagnetic field accompanying the partial solar eclipse over Kharkov are presented. The ionospheric effects have been studied with the use of an ionosonde and measurements of the phase and amplitude of a radio signal with a frequency of 66.(6) kHz on the Moscow–Kharkov route, and the effects in the magnetic field have been analyzed with the help of a magnetometer–fluxmeter in the range of periods from 1 to 1000 s. Disturbances in both the lower and middle ionosphere, as well as in the geomagnetic field, have been detected. The observation results have been compared with the results of a simulation of physical processes accompanying the solar eclipse. A good agreement has been found between observational and modeling results.  相似文献   

Rise of a Meteoroid Thermal in the Earth’s Atmosphere     

L.?F.?ChernogorEmail author  Yu.?B.?Mylovanov 《Kinematics and Physics of Celestial Bodies》2018,34(4):198-206

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Melting relations of multicomponent carbonate MgCO3–FeCO3–CaCO3–Na2CO3 system at 12–26 GPa: application to deeper mantle diamond formation     

Anna Spivak  Natalia Solopova  Leonid Dubrovinsky  Yuriy Litvin 《Physics and Chemistry of Minerals》2015,42(10):817-824

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Atomic arrangements around the O3 site in Al- and Cr-rich oxy-tourmalines: a combined EMP,SREF, FTIR and Raman study     

Ferdinando Bosi  Henrik Skogby  Peter Lazor  Leonid Reznitskii 《Physics and Chemistry of Minerals》2015,42(6):441-453

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Gravitational diffusion in the intracluster medium     

Leonid Chuzhoy  Adi Nusser 《Monthly notices of the Royal Astronomical Society》2003,342(1):L5-L8

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Major element and primary sulfur concentrations in Apollo 12 mare basalts: The view from melt inclusions     

Daniel J. BOMBARDIERI  Marc D. NORMAN  Vadim S. KAMENETSKY  Leonid V. DANYUSHEVSKY 《Meteoritics & planetary science》2005,40(5):679-693

Abstract— Major element and sulfur concentrations have been determined in experimentally heated olivine‐hosted melt inclusions from a suite of Apollo 12 picritic basalts (samples 12009, 12075, 12020, 12018, 12040, 12035). These lunar basalts are likely to be genetically related by olivine accumulation (Walker et al. 1976a, b). Our results show that major element compositions of melt inclusions from samples 12009, 12075, and 12020 follow model crystallization trends from a parental liquid similar in composition to whole rock sample 12009, thereby partially confirming the olivine accumulation hypothesis. In contrast, the compositions of melt inclusions from samples 12018, 12040, and 12035 fall away from model crystallization trends, suggesting that these samples crystallized from melts compositionally distinct from the 12009 parent liquid and therefore may not be strictly cogenetic with other members of the Apollo 12 picritic basalt suite. Sulfur concentrations in melt inclusions hosted in early crystallized olivine (Fo₇₅) are consistent with a primary magmatic composition of 1050 ppm S, or about a factor of 2 greater than whole rock compositions with 400–600 ppm S. The Apollo 12 picritic basalt parental magma apparently experienced outgassing and loss of S during transport and eruption on the lunar surface. Even with the higher estimates of primary magmatic sulfur concentrations provided by the melt inclusions, the Apollo 12 picritic basalt magmas would have been undersaturated in sulfide in their mantle source regions and capable of transporting chalcophile elements from the lunar mantle to the surface. Therefore, the measured low concentration of chalcophile elements (e.g., Cu, Au, PGEs) in these lavas must be a primary feature of the lunar mantle and is not related to residual sulfide remaining in the mantle during melting. We estimate the sulfur concentration of the Apollo 12 mare basalt source regions to be ～75 ppm, which is significantly lower than that of the terrestrial mantle.  相似文献   

Technogenic hydrogeochemical anomalies of tungsten deposits in Kykylbey ore region     

LeonidV.Zamana LarisaP.Chechel 《东北亚地学研究》2004,7(1):52-57

Peculiarities of the tungsten deposits drainage flow chemical composition formation, the development of which was ceased almost 40 years ago, have been considered. Migration peculiarities of ore components have been covered, and forms of their migration have been calculated. Inertial characteristics of the surface flow contamination are shown.  相似文献