183 research outputs found
Ar-40 to Ar-39 ages of the large impact structures Kara and Manicouagan and their relevance to the Cretaceous-Tertiary and the Triassic-Jurassic boundary
Since the discovery of the Ir enrichment in Cretaceous-Tertiary boundary clays in 1980, the effects of a 10-km asteroid impacting on the Earth 65 Ma ago have been discussed as the possible reason for the mass extinction--including the extinction of the dinosaurs--at the end of the Cretaceous. But up to now no crater of this age that is large enough (ca. 200 km in diameter) has been found. One candidate is the Kara Crater in northern Siberia. Kolesnikov et al. determined a K-Ar isochron of 65.6 +/- 0.5 Ma, indistinguishable from the age of the K-T boundary and interpreted this as confirmation of earlier proposals that the Kara bolide would have been at least one of the K-T impactors. Koeberl et al. determined Ar-40 to Ar-39 ages ranging from 70 to 82 Ma and suggested an association to the Campanian-Maastrichtian boundary, another important extinction horizon 73 Ma ago. We dated four impact melts, KA2-306, KA2-305, SA1-302, and AN9-182. Results from the investigation are discussed
Early Thermal Evolution of Planetesimals and its Impact on Processing and Dating of Meteoritic Material
Radioisotopic ages for meteorites and their components provide constraints on
the evolution of small bodies: timescales of accretion, thermal and aqueous
metamorphism, differentiation, cooling and impact metamorphism. Realising that
the decay heat of short-lived nuclides (e.g. 26Al, 60Fe), was the main heat
source driving differentiation and metamorphism, thermal modeling of small
bodies is of utmost importance to set individual meteorite age data into the
general context of the thermal evolution of their parent bodies, and to derive
general conclusions about the nature of planetary building blocks in the early
solar system. As a general result, modelling easily explains that iron
meteorites are older than chondrites, as early formed planetesimals experienced
a higher concentration of short-lived nuclides and more severe heating.
However, core formation processes may also extend to 10 Ma after formation of
Calcium-Aluminum-rich inclusions (CAIs). A general effect of the porous nature
of the starting material is that relatively small bodies (< few km) will also
differentiate if they form within 2 Ma after CAIs. A particular interesting
feature to be explored is the possibility that some chondrites may derive from
the outer undifferentiated layers of asteroids that are differentiated in their
interiors. This could explain the presence of remnant magnetization in some
chondrites due to a planetary magnetic field.Comment: 24 pages, 9 figures, Accepted for publication as a chapter in
Protostars and Planets VI, University of Arizona Press (2014), eds. H.
Beuther, R. Klessen, C. Dullemond, Th. Hennin
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Isheyevo Meteorite: Genetic link between CH and CB chondrites?
Based on the mineralogy, petrography, bulk chemical, oxygen, and nintrogen isotopic compositions and 40Ar-39Ar age, Isheyevo is genetically related to CH and CB carbonaceous chondrites and provides a link between these group of pristine meteorites
Ar-40 to Ar-39 dating of pseudotachylites from the Witwatersrand basin, South Africa, with implications for the formation of the Vredefort Dome
The formation of the Vredefort Dome, a structure in excess of 100 km in diameter and located in the approximate center of the Witwatersrand basin, is still the subject of lively geological controversy. It is widely accepted that its formation seems to have taken place in a single sudden event, herein referred to as the Vredefort event, accompanied by the release of gigantic amounts of energy. It is debated, however, whether this central event was an internal one, i.e., a cryptoexplosion triggered by volcanic or tectonic processes, or the impact of an extraterrestrial body. The results of this debate are presented
The formation of the solar system
The solar system started to form about 4.56 Gyr ago and despite the long
intervening time span, there still exist several clues about its formation. The
three major sources for this information are meteorites, the present solar
system structure and the planet-forming systems around young stars. In this
introduction we give an overview of the current understanding of the solar
system formation from all these different research fields. This includes the
question of the lifetime of the solar protoplanetary disc, the different stages
of planet formation, their duration, and their relative importance. We consider
whether meteorite evidence and observations of protoplanetary discs point in
the same direction. This will tell us whether our solar system had a typical
formation history or an exceptional one. There are also many indications that
the solar system formed as part of a star cluster. Here we examine the types of
cluster the Sun could have formed in, especially whether its stellar density
was at any stage high enough to influence the properties of today's solar
system. The likelihood of identifying siblings of the Sun is discussed.
Finally, the possible dynamical evolution of the solar system since its
formation and its future are considered.Comment: 36 pages, 7 figures, invited review in Physica Script
Distribution of mantle and atmospheric argon in mantle xenoliths from the Western Arabian peninsula: Constraints on timing and composition of metasomatizing agents in the lithospheric mantle
To investigate the geochemical behaviour of argon isotopes during mantle metasomatism and to obtain chronological information on the age of metasomatic events under the Arabian Shield, we analyzed mantle xenoliths and hornblende megacrysts from Saudi Arabian volcanic fields (Uwayrid, Al Birk) applying the 40Ar-39Ar dating technique. Two hornblende megacrysts yield plateau ages indicating formation or total resetting of the K/Ar system 1-2 Myr ago. The ultramafic xenoliths trapped mantle-derived and atmospheric argon in different proportions, resulting in variable isotopic compositions: 40Ar/36Ar ratios range from 296 (i.e. atmospheric) to 10 500, reflecting interactions with isotopically and genetically different fluids and/or melts during recent mantle metasomatism. One such episode of metasomatism led to the formation of Ba-rich phlogopite, which yielded a saddle-shaped age spectrum with a maximum age estimate of 18 Ma. Another episode, inducing formation of secondary pargasite in the lithospheric mantle, was dated to 4 Ma. In the mantle xenoliths the concentration of mantle argon is clearly related to the intensity of metasomatism. Argon extraction by high-resolution stepwise heating allowed us to deconvolve various argon components distributed heterogeneously within single xenoliths and ascribe them to specific carrier phases. Pyroxenes generally preserve much higher 40Ar/36Ar ratios than olivine, as they contain up to 100 times higher concentrations of mantle argon, which also correlates with a higher fluid inclusion content in pyroxenes. Hydrous phases (phlogopite/amphibole) have more variable 40Ar/36Ar ratios. K and Cl concentrations and the argon isotope compositions of the Uwayrid xenoliths indicate distinct metasomatic agents, causing elemental and isotopic disequilibrium on a local scale. On the basis of correlations between Ar isotope composition and K and Cl concentration in the samples most strongly affected by the late metasomatic fluids, we suggest that metasomatic processes in the local mantle occurring simultaneously with the opening of the Red Sea were accompanied by the introduction of saline-water saturated fluids into deep lithospheric zones
Thermal history modeling of the H chondrite parent body
The cooling histories of individual meteorites can be empirically
reconstructed by using ages from different radioisotopic chronometers with
distinct closure temperatures. For a group of meteorites derived from a single
parent body such data permit the reconstruction of the cooling history and
properties of that body. Particularly suited are H chondrites because precise
radiometric ages over a wide range of closure temperatures are available. A
thermal evolution model for the H chondrite parent body is constructed by using
all H chondrites for which at least three different radiometric ages are
available. Several key parameters determining the thermal evolution of the H
chondrite parent body and the unknown burial depths of the H chondrites are
varied until an optimal fit is obtained. The fit is performed by an 'evolution
algorithm'. Empirical data for eight samples are used for which radiometric
ages are available for at least three different closure temperatures. A set of
parameters for the H chondrite parent body is found that yields excellent
agreement (within error bounds) between the thermal evolution model and
empirical data of six of the examined eight chondrites. The new thermal model
constrains the radius and formation time of the H chondrite parent body
(possibly (6) Hebe), the initial burial depths of the individual H chondrites,
the average surface temperature of the body, the average initial porosity of
the material the body accreted from, and the initial 60Fe content of the H
chondrite parent body.Comment: 16 pages, 7 figure
Π Π΅Π·ΡΠ»ΡΡΠ°ΡΡ ΡΠ΅ΠΎΡΠ΅ΡΠΈΡΠ΅ΡΠΊΠΈΡ ΠΈ ΠΎΠΏΡΡΠ½ΡΡ ΡΠ°Π±ΠΎΡ ΠΏΠΎ ΠΈΠ·ΡΡΠ΅Π½ΠΈΡ ΠΌΠ΅Ρ Π°Π½ΠΈΠ·ΠΌΠ° ΡΠ°Π±ΠΎΡΡ Π±ΡΡΠΎΠ²ΡΡ ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΠΌΠ°ΡΡ ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ
ΠΠΊΡΡΠ°Π»ΡΠ½ΠΎΡΡΡ ΡΠ°Π±ΠΎΡΡ: Π½Π΅ΠΎΠ±Ρ
ΠΎΠ΄ΠΈΠΌΠΎΡΡΡ ΠΏΠΎΠ²ΡΡΠ΅Π½ΠΈΡ ΡΡΡΠ΅ΠΊΡΠΈΠ²Π½ΠΎΡΡΠΈ Π±ΡΡΠ΅Π½ΠΈΡ Π³Π΅ΠΎΠ»ΠΎΠ³ΠΎΡΠ°Π·Π²Π΅Π΄ΠΎΡΠ½ΡΡ
ΡΠΊΠ²Π°ΠΆΠΈΠ½ Π² ΡΠ»ΠΎΠΆΠ½ΡΡ
Π³ΠΎΡΠ½ΠΎ-Π³Π΅ΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΡΠ»ΠΎΠ²ΠΈΡΡ
, Π² ΡΠΎΠΌ ΡΠΈΡΠ»Π΅ ΡΠ²ΡΠ·Π°Π½Π½ΡΡ
Ρ Π΅ΡΡΠ΅ΡΡΠ²Π΅Π½Π½ΡΠΌ ΠΈΡΠΊΡΠΈΠ²Π»Π΅Π½ΠΈΠ΅ΠΌ ΡΠΊΠ²Π°ΠΆΠΈΠ½. Π¦Π΅Π»Ρ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ: ΡΠ°Π·ΡΠ°Π±ΠΎΡΠΊΠ° ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊΠΈ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ ΠΈ ΠΊΠΎΠ½ΡΡΡΡΠΊΡΠΈΠΉ Π±ΡΡΠΎΠ²ΡΡ
ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΠΌΠ°ΡΡ (ΡΡΠΆΠ΅ΡΡΠΈ) ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ, ΠΏΠΎΠ·Π²ΠΎΠ»ΡΡΡΠΈΡ
ΠΏΠΎΠ²ΡΡΠΈΡΡ ΡΡΡΠ΅ΠΊΡΠΈΠ²Π½ΠΎΡΡΡ Π±ΡΡΠ΅Π½ΠΈΡ Π³Π΅ΠΎΠ»ΠΎΠ³ΠΎΡΠ°Π·Π²Π΅Π΄ΠΎΡΠ½ΡΡ
ΡΠΊΠ²Π°ΠΆΠΈΠ½. ΠΠ΅ΡΠΎΠ΄Ρ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ: Π°Π½Π°Π»ΠΈΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ, ΠΎΠΏΡΡΠ½ΠΎ-ΠΊΠΎΠ½ΡΡΡΡΠΊΡΠΎΡΡΠΊΠΈΠ΅ ΡΠ°Π±ΠΎΡΡ ΠΈ ΡΠΊΡΠΏΠ΅ΡΠΈΠΌΠ΅Π½ΡΠ°Π»ΡΠ½ΡΠ΅ ΠΎΠΏΡΡΠ½ΡΠ΅ ΡΠ°Π±ΠΎΡΡ. Π Π΅Π·ΡΠ»ΡΡΠ°ΡΡ. Π Π°Π·ΡΠ°Π±ΠΎΡΠ°Π½Ρ ΡΠ΅ΠΎΡΠ΅ΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ ΠΏΠΎΠ»ΠΎΠΆΠ΅Π½ΠΈΡ, ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊΠ° ΠΏΡΠΈΠΌΠ΅Π½Π΅Π½ΠΈΡ ΠΈ ΠΊΠΎΠ½ΡΡΡΡΠΊΡΠΈΠΈ Π±ΡΡΠΎΠ²ΡΡ
ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ; ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½Ρ ΠΏΡΠΎΠΈΠ·Π²ΠΎΠ΄ΡΡΠ²Π΅Π½Π½ΡΠ΅ ΠΈΡΠΏΡΡΠ°Π½ΠΈΡ ΡΠ°Π·Π»ΠΈΡΠ½ΡΡ
ΠΊΠΎΠ½ΡΡΡΡΠΊΡΠΈΠΉ Π±ΡΡΠΎΠ²ΡΡ
ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ ΠΏΡΠΈ ΡΠ°Π·Π»ΠΈΡΠ½ΡΡ
ΡΠΏΠΎΡΠΎΠ±Π°Ρ
Π±ΡΡΠ΅Π½ΠΈΡ. ΠΡΠ²ΠΎΠ΄Ρ. ΠΠ° ΠΎΡΠ½ΠΎΠ²Π΅ ΡΠ°Π·ΡΠ°Π±ΠΎΡΠ°Π½Π½ΠΎΠΉ ΠΌΠΎΠ΄Π΅Π»ΠΈ Π΄Π²ΠΈΠΆΠ΅Π½ΠΈΡ Π±ΡΡΠΎΠ²ΡΡ
ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ ΠΏΠΎΠ»ΡΡΠ΅Π½Ρ Π°Π½Π°Π»ΠΈΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ Π·Π°Π²ΠΈΡΠΈΠΌΠΎΡΡΠΈ Π΄Π»Ρ ΡΠ°ΡΡΠ΅ΡΠ° Π²Π΅Π»ΠΈΡΠΈΠ½ ΡΠΊΡΡΠ΅Π½ΡΡΠΈΡΠΈΡΠ΅ΡΠ° ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ Π±ΡΡΠΎΠ²ΡΡ
ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΎΠΊ, ΠΎΠ±Π΅ΡΠΏΠ΅ΡΠΈΠ²Π°ΡΡΠΈΠ΅ ΠΈΡ
Π²ΡΠ°ΡΠ΅Π½ΠΈΠ΅ Π²ΠΎΠΊΡΡΠ³ ΠΎΡΠΈ ΡΠΊΠ²Π°ΠΆΠΈΠ½Ρ (Π²ΠΈΠ΄ Π€1), Π° ΡΠ°ΠΊΠΆΠ΅ Π΄Π»ΠΈΠ½Ρ Π²ΠΎΠ²Π»Π΅ΠΊΠ°Π΅ΠΌΠΎΠ³ΠΎ Π² ΡΠ΅ΠΆΠΈΠΌ Π²ΡΠ°ΡΠ΅Π½ΠΈΡ Π€1 ΡΡΠ°ΡΡΠΊΠ° ΠΊΠΎΠ»ΠΎΠ½Π½Ρ, ΡΡΠΎ ΠΏΠΎΠ·Π²ΠΎΠ»ΡΠ΅Ρ ΡΠΎΠ·Π΄Π°Π²Π°ΡΡ ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΊΠΈ Π±ΡΡΠΈΠ»ΡΠ½ΠΎΠΉ ΠΊΠΎΠ»ΠΎΠ½Π½Ρ, ΡΠΏΠΎΡΠΎΠ±Π½ΡΠ΅ ΡΠ°Π±ΠΎΡΠ°ΡΡ Π² Π±ΠΎΠ»Π΅Π΅ Π±Π»Π°Π³ΠΎΠΏΡΠΈΡΡΠ½ΠΎΠΌ ΡΠ΅ΠΆΠΈΠΌΠ΅ ΠΈ ΠΎΠ±Π΅ΡΠΏΠ΅ΡΠΈΠ²Π°ΡΡ ΠΏΠΎΠ²ΡΡΠ΅Π½ΠΈΠ΅ ΡΡΡΠ΅ΠΊΡΠΈΠ²Π½ΠΎΡΡΠΈ Π±ΡΡΠΎΠ²ΠΎΠ³ΠΎ ΠΏΡΠΎΡΠ΅ΡΡΠ°. ΠΠ° ΠΎΡΠ½ΠΎΠ²Π΅ ΡΡΠ°Π½Π΄Π°ΡΡΠ½ΡΡ
ΡΠ½Π°ΡΡΠ΄ΠΎΠ² ΡΠΎ ΡΡΠ΅ΠΌΠ½ΡΠΌ ΠΊΠ΅ΡΠ½ΠΎΠΏΡΠΈΠ΅ΠΌΠ½ΠΈΠΊΠΎΠΌ ΡΠΈΠΏΠΎΡΠ°Π·ΠΌΠ΅ΡΠ° HQ ΡΠ°Π·ΡΠ°Π±ΠΎΡΠ°Π½Ρ ΠΈ ΠΈΠ·Π³ΠΎΡΠΎΠ²Π»Π΅Π½Ρ ΡΡΡΠ±Ρ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ, ΠΊΠΎΡΠΎΡΡΠ΅ ΠΈΡΠΏΡΡΠ°Π½Ρ Π½Π° ΠΏΡΠΎΠΈΠ·Π²ΠΎΠ΄ΡΡΠ²Π΅Π½Π½ΡΡ
ΡΠΊΠ²Π°ΠΆΠΈΠ½Π°Ρ
Π² ΡΠΎΡΡΠ°Π²Π΅ ΠΊΠΎΠΌΠΏΠΎΠ½ΠΎΠ²ΠΊΠΈ, Π² ΠΊΠΎΡΠΎΡΠΎΠΉ ΡΠ°Π·ΠΌΠ΅ΡΠ΅Π½ΠΎ ΡΡΠΈ ΡΡΡΠ±Ρ ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ ΠΏΠΎΠΏΠ΅ΡΠ΅ΡΠ½ΠΎΠ³ΠΎ ΡΠ΅ΡΠ΅Π½ΠΈΡ. Π Π΅Π·ΡΠ»ΡΡΠ°ΡΡ ΠΈΡΠΏΡΡΠ°Π½ΠΈΠΉ ΠΏΠΎΠΊΠ°Π·Π°Π»ΠΈ, ΡΡΠΎ Π² ΡΠΎΡΡΠ°Π²Π΅ Π²ΡΡΠΎΠΊΠΎΡΠ±Π°Π»Π°Π½ΡΠΈΡΠΎΠ²Π°Π½Π½ΡΡ
Π±ΡΡΠΈΠ»ΡΠ½ΡΡ
ΠΊΠΎΠ»ΠΎΠ½Π½ ΡΠ½Π°ΡΡΠ΄Π° ΡΠΎ ΡΡΠ΅ΠΌΠ½ΡΠΌ ΠΊΠ΅ΡΠ½ΠΎΠΏΡΠΈΠ΅ΠΌΠ½ΠΈΠΊΠΎΠΌ ΡΡΡΠ΅ΠΊΡΠΈΠ²Π½ΠΎ ΠΏΡΠΈΠΌΠ΅Π½Π΅Π½ΠΈΠ΅ ΡΡΡΠ± ΡΠΎ ΡΠΌΠ΅ΡΠ΅Π½Π½ΡΠΌ ΡΠ΅Π½ΡΡΠΎΠΌ ΡΡΠΆΠ΅ΡΡΠΈ: Π΄ΠΎΡΡΠΈΠ³Π°Π΅ΡΡΡ ΡΠ½ΠΈΠΆΠ΅Π½ΠΈΠ΅ ΠΈΠ½ΡΠ΅Π½ΡΠΈΠ²Π½ΠΎΡΡΠΈ Π΅ΡΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ³ΠΎ ΠΈΡΠΊΡΠΈΠ²Π»Π΅Π½ΠΈΡ ΡΠΊΠ²Π°ΠΆΠΈΠ½, ΡΠ½ΠΈΠΆΠ°Π΅ΡΡΡ Π²ΠΈΠ±ΡΠ°ΡΠΈΡ ΠΈ Π·Π°ΡΡΠ°ΡΡ ΠΌΠΎΡΠ½ΠΎΡΡΠΈ Π½Π° ΡΠ°Π±ΠΎΡΡ Π±ΡΡΠΈΠ»ΡΠ½ΠΎΠΉ ΠΊΠΎΠ»ΠΎΠ½Π½Ρ.Relevance of the research is the necessity to increase the efficiency of drilling prospecting wells in difficult mining-and-geological conditions, including those connected with a natural curvature of wells. The aim of the research is to develop a technique of using and designs of boring configurations with the displaced cross section mass center which allow increasing the efficiency of drilling the prospecting wells. Research methods: analytical researches, developmental works and experimental skilled works. Results. The authors have developed the theoretical regulations, a technique of application and a design of boring configurations with the displaced cross section mass center and carried out the production tests of various designs of boring configurations of with the displaced cross section mass center when drilling. Conclusions. Based on the developed model of movement of boring configurations with the displaced center of gravity of cross section the authors obtained the analytical dependences for calculating the sizes of eccentricity of boring configuration cross section providing their rotation round a well axis (Π€1 type), as well as the length of the column part involved in the rotation mode Π€1 that allows developing the configurations of a boring column capable of operating in more favorable mode and providing the increase of boring efficiency. Based on standard shells with the removable core receiver of a standard size of HQ the pipes with the displaced cross section mass center were developed and produced. They were tested on production wells as a part of configuration in which three pipes with the displaced cross section mass center were placed. The results of the tests showed that it is efficient to apply the pipes with the displaced cross section mass center as a part of the high-balanced boring columns as the decrease in intensity of natural curvature of wells is reached, vibration and costs of power for boring column operation decrease
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