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1.
V. S. Kulikov Ya. V. Bychkova V. V. Kulikova Yu. A. Kostitsyn O. S. Pokrovsky M. V. Vasil’ev 《Petrology》2008,16(6):531-551
The Ruiga differentiated mafic-ultramafic intrusion in the northwestern part of the Vetreny Belt paleorift was described for the first time based on geological, petrological, geochronological, and geochemical data. The massif (20 km2 in exposed area) is a typical example of shallow-facies peridotite-gabbro-komatiite-basalt associations and consists of three zones up to 810 m in total thickness (from bottom to top): melanogab-bronorite, peridotite, and gabbro. In spite of pervasive greenschist metamorphism, the rocks contain locally preserved primary minerals: olivine (Fo 75–86), bronzite, augite of variable composition, labradorite, and Cr-spinels. A mineral Sm-Nd isochron on olivine melanogabbronorite from the Ruiga Massif defines an age of 2.39 ± 0.05 Ga, while komatiitic basalts of the Vetreny Belt Formation were dated at 2.40–2.41 Ga (Puchtel et al., 1997). The rocks of the Ruiga intrusion and lava flows of Mt. Golets have similar major, rare-earth, and trace element composition, which suggests their derivation from a single deep-seated source. Their parent magma was presumably a high-Mg komatiitic basalt. In transitional crustal chambers, its composition was modified by olivine-controlled fractionation and crustal contamination, with the most contaminated first portions of the ejected melt. In terms of geology and geochemistry, the considered magmatic rocks of the Vetreny Belt are comparable with the Raglan Ni-PGE komatiite gabbro-peridotite complex in Canada (Naldrett, 2003). 相似文献
2.
From long-term observations of ozone evolution in the stratosphere of the Kola Peninsula in the 2002/2003 winter, the rates of chemical destruction of ozone and its net loss at isentropic levels of 530 K (an altitude of about 22 km) and 465 K (an altitude of about 19 km) ar evaluated with consideration for diabatic descent of air masses. These rates were ?18.6±3.3 and ?14.3±2.9 ppb/day and the net loss of ozone due to its chemical destruction over the period from December 1, 2002, to March 5, 2003, reached 1.77±0.33 ppm and 1.36±0.29 ppm, respectively. At the lower level, these data are in satisfactory agreement (to within measurement errors) with other measurements that were taken at that time. At a potential-temperature level of 530 K, the ozone loss in the 2002/2003 season evaluated from our data and from similar microwave measurements performed in Kiruna (Sweden) virtually coincides and testifies to the fact that the net loss increases with altitude. These inferences are inconsistent with the results obtained with the Match technique and the method of averaging over a vortex, which indicate that the ozone loss decreases with altitude. However, since polar stratospheric clouds were detected regularly in December and early January at levels up to 600 K or higher, it may be suggested that the ozone loss at these altitudes can be comparable to the values found for isentropic levels of 465 to 475 K. 相似文献
3.
Kulikov V. A. Ionicheva A. P. Kolodyazhny S. Yu. Sokolova E. Yu. Pushkarev P. Yu. Yakovlev A. G. 《Izvestiya Physics of the Solid Earth》2022,58(5):642-654
Izvestiya, Physics of the Solid Earth - Abstract—The paper presents results of magnetotelluric sounding performed in the South-Eastern Ladoga Region in 2018–2021 for the purpose of... 相似文献
4.
Yu. Yu. Kulikov A. A. Krasil’nikov V. M. Demkin V. G. Ryskin 《Izvestiya Atmospheric and Oceanic Physics》2008,44(4):486-490
We present the results of microwave observations of the ozone content variability in the upper stratosphere and lower mesosphere during a total solar eclipse of March 29, 2006 at the Kislovodsk high-altitude scientific station. An increase in the concentration of mesospheric ozone was recorded during the eclipse. At a height of 60 km, the ozone concentration increased by 40%, which is close to the value of diurnal ozone variations. 相似文献
5.
Recent results of Milagro, Tibet, ARGO-YBJ, and IceCube experiments on the small-scale anisotropy of Galactic cosmic rays (CRs) with energies from units up to a few hundred TeV arise a question on a possible nature of the observed phenomenon, as well as on the anisotropy of CRs at higher energies. An analysis of a small-scale anisotropy of CRs with energies at around PeV registered with the EAS MSU array presented in the article, reveals a number of regions with an excessive flux. A typical size of the regions varies from 3° up to 12°. We study correlation of these regions with positions of potential astrophysical sources of CRs and discuss a possible origin of the observed anisotropy. 相似文献
6.
Kulikov G. V. Spector S. V. Rogozhin E. A. Lukashova R. N. Sysolin A. I. 《Izvestiya Atmospheric and Oceanic Physics》2019,55(11):1715-1725
Izvestiya, Atmospheric and Oceanic Physics - The permanent analysis of the hydrogeodeformation (HGD) field is one promising direction in the field of predicting strong earthquakes. As a result of... 相似文献
7.
Leitzinger M Odert P Kulikov YN Lammer H Wuchterl G Penz T Guarcello MG Micela G Khodachenko ML Weingrill J Hanslmeier A Biernat HK Schneider J 《Planetary and Space Science》2011,59(13):1472-1481
We present thermal mass loss calculations over evolutionary time scales for the investigation if the smallest transiting rocky exoplanets CoRoT-7b (∼1.68REarth) and Kepler-10b (∼1.416REarth) could be remnants of an initially more massive hydrogen-rich gas giant or a hot Neptune-class exoplanet. We apply a thermal mass loss formula which yields results that are comparable to hydrodynamic loss models. Our approach considers the effect of the Roche lobe, realistic heating efficiencies and a radius scaling law derived from observations of hot Jupiters. We study the influence of the mean planetary density on the thermal mass loss by placing hypothetical exoplanets with the characteristics of Jupiter, Saturn, Neptune, and Uranus to the orbital location of CoRoT-7b at 0.017 AU and Kepler-10b at 0.01684 AU and assuming that these planets orbit a K- or G-type host star. Our findings indicate that hydrogen-rich gas giants within the mass domain of Saturn or Jupiter cannot thermally lose such an amount of mass that CoRoT-7b and Kepler-10b would result in a rocky residue. Moreover, our calculations show that the present time mass of both rocky exoplanets can be neither a result of evaporation of a hydrogen envelope of a “Hot Neptune” nor a “Hot Uranus”-class object. Depending on the initial density and mass, these planets most likely were always rocky planets which could lose a thin hydrogen envelope, but not cores of thermally evaporated initially much more massive and larger objects. 相似文献
8.
H. Lammer V. Eybl K. G. Kislyakova J. Weingrill M. Holmstr?m M. L. Khodachenko Yu. N. Kulikov A. Reiners M. Leitzinger P. Odert M. Xiang?Gr��? B. Dorner M. G��del A. Hanslmeier 《Astrophysics and Space Science》2011,335(1):39-50
The detection and investigation of EUV heated, extended and non-hydrostatic upper atmospheres around terrestrial exoplanets would provide important insights into the interaction of the host stars plasma environment as well as the evolution of Earth-type planets their atmospheres and possible magnetic environments. We discuss different scenarios where one can expect that Earth-like planets should experience non-hydrostatic upper atmosphere conditions so that dynamically outward flowing neutral atoms can interact with the stellar plasma flow so that huge hydrogen coronae and energetic neutral atoms (ENA) can be produced via charge exchange. By observing the size of the extended upper atmospheres and related ENA-clouds and by determining the velocities of the surrounding hydrogen atoms, conclusions can be drawn in respect to the origin of these features. Due to the large number of M-type stars in our neighbourhood and their long periods of strong and moderate stellar activity in comparison to G-stars, we expect that M-type stars represent the most promising candidates for the detection of hydrogen ENA-clouds and the subsequent study of the interaction between the host star and the planets?? upper atmosphere. We show that the low mass of M-type stars also makes them preferable targets to observe extended hydrogen clouds around terrestrial exoplanets with a mass as low as one Earth mass. Transit follow-up observations in the UV-range of terrestrial exoplanets around M-type stars with space observatories such as the World Space Observatory-UV (WSO-UV) would provide a unique opportunity to shed more light on the early evolution of Earth-like planets, including those of our own Solar System. 相似文献
9.
M. I. Beloglazov V. M. Demkin A. A. Krasilnikov L. M. Kukin Yu. Yu. Kulikov V. G. Ryskin V. N. Shanin 《Geomagnetism and Aeronomy》2010,50(2):256-262
As a result of the long-term observations lead in region of Kola Peninsula, connection between character of variations of
the ozone content in a stratosphere of Arctic regions and behavior and structure of a winter polar vortex is established.
During winter seasons with well developed cyclone and duration of stable existence not less than 1.5–2 months were observed
extremely low ozone number density at heights 20–25 km connected, apparently, with its chemical destruction. On the other
hand, during disturbances of the vortex, accompanied strong stratospheric warming, was registered almost double increase of
ozone amount in a high-altitude interval from 20 up to 40 km. Comparison of results of ground-based microwave monitoring of
an ozone layer to data of the satellite instrument EOS MLS installed on satellite AURA is lead. In most cases comparison has
shown satisfactory within the limits of an error of measurements coincidence of results. However in conditions of atmospheric
disturbances when arose significant spatial heterogeneity, the discrepancy of results of comparison was marked. The possible
reasons which cause the detected disagreement in results are discussed. 相似文献
10.