83 research outputs found
Reflection of hydrogen and deuterium atoms from the beryllium, carbon, tungsten surfaces
Particle reflection coefficients for scattering of hydrogen and deuterium atoms from amorphous beryllium, carbon and tungsten were obtained, which are of interest for thermonuclear reactor physics. For the case of deuterium scattering from tungsten the data were also calculated for polycrystalline and crystalline target. The calculations were carried out by two methods: by modeling the trajectories of the incident particles and by using the binary collision approximation. Interaction potentials between hydrogen and helium atoms and the selected materials were calculated in the scope of the density function theory using program DMol for choosing wave functions. The dependence of the reflection coefficient RN on the potential well depth was found. The results demonstrate a good agreement with the available experimental values.Peer reviewe
Two new bright Ae stars
Two newly identified Ae stars, nu Cyg and kappa UMa, were discovered in the
course of the Magnetic Survey of Bright MS stars (Monin et al. 2002). We pre
sent their Halpha profiles along with measurements of their equivalent width
and parameters of emission features. Emission in the Halpha line of nu Cyg is
variable on a time scale of 3 years. kappa UMa exhibits weak emission which is
rather stable. The emission is thought to arise from a circumstellar disk, and
we have estimated the size of that disk.Both new emission stars are IRAS
sources. Their IR color excesses are consistent with those of classical Ae
stars. Thus, nu Cyg and kappa UMa appear not to belong to the class of Herbig
Ae/Be stars. We argue that the frequency of Ae stars may be underestimated due
to the difficulty of detection of weak emission in some A stars.Comment: 6 pages,3 figures, submitted to A&
Low-Surface-Brightness Galaxies in the Sloan Digital Sky Survey. I. Search Method and Test Sample
In this paper we present results of a pilot study to use imaging data from
the Sloan Digital Sky Survey (SDSS) to search for low-surface-brightness (LSB)
galaxies. For our pilot study we use a test sample of 92 galaxies from the
catalog of Impey et al. (1996) distributed over 93 SDSS fields of the Early
Data Release (EDR). Many galaxies from the test sample are either LSB or dwarf
galaxies. To deal with the SDSS data most effectively a new photometry software
was created, which is described in this paper. We present the results of the
selection algorithms applied to these 93 EDR fields. Two galaxies from the
Impey et al. test sample are very likely artifacts, as confirmed by follow-up
imaging. With our algorithms, we were able to recover 87 of the 90 remaining
test sample galaxies, implying a detection rate of 96.5%. The three
missed galaxies fall too close to very bright stars or galaxies. In addition,
42 new galaxies with parameters similar to the test sample objects were found
in these EDR fields (i.e., 47% additional galaxies). We present the main
photometric parameters of all identified galaxies and carry out first
statistical comparisons. We tested the quality of our photometry by comparing
the magnitudes for our test sample galaxies and other bright galaxies with
values from the literature. All these tests yielded consistent results. We
briefly discuss a few unusual galaxies found in our pilot study, including an
LSB galaxy with a two-component disk and ten new giant LSB galaxies.Comment: 36 pages, 16 figures, accepted for publication by AJ, some figures
were bitmapped to reduce the siz
Discovery of Eight New Extremely Metal--Poor Galaxies in the Sloan Digital Sky Survey
We report the discovery of eight new extremely metal-poor galaxies (XMPGs;
12+log(O/H) < 7.65) and the recovery of four previously known or suspected
XMPGs (IZw18, HS0822+3542, HS0837+4717 and A1116+517) using Sloan Digital Sky
Survey (SDSS) spectroscopy. These new objects were identified after an analysis
of 250,000 galaxy spectra within an area of ~3000 deg^2 on the sky. Our oxygen
abundance determinations have an accuracy of 0.1 dex and are based on the
temperature-sensitive [O {\sc iii}] 4363 \AA line and on the direct
calculation of the electron temperature. We briefly discuss a new method of
oxygen abundance determinations using the [O {\sc ii}] 7319,7330 \AA\
lines, which is particularly useful for SDSS emission-line spectra with
redshifts ~0.024 since the [O {\sc ii}] 3727 \AA emission line
falls outside of the SDSS wavelength range. We detect XMPGs with redshifts
ranging from 0.0005 to 0.0443 and luminosities from 12\fm4 to
18\fm6. Our eight new XMPGs increase the number of known metal-deficient
galaxies by approximately one quarter. The estimated surface density of XMPGs
is 0.004 deg for 17\fm77.Comment: To appear in August 20 issue of ApJ Letters, 6 pages, 2 figure
The metallicities of UM151, UM408 and A1228+12 revisited
We present the results of new spectrophotometry and heavy element abundance
determinations for 3 dwarf galaxies UM151, UM408 and A1228+12 (RMB132). These
galaxies have been claimed in the literature to have very low metallicities,
corresponding to log(O/H)+12 < 7.65, that are in the metallicity range of some
candidate local young galaxies. We present higher S/N data for these three
galaxies. UM151 and UM408 have significantly larger metallicities: log(O/H)+12
= 8.5 and 7.93, respectively. For A1228+12 our new log(O/H)+12 = 7.73 is close
to that recalculated from earlier data (7.68). Thus, the rederived
metallicities allow us to remove these objects from the list of galaxies with Z
< 1/20 Z_Sun.Comment: LaTeX, 8 pages with 3 Postscript figures, A&A in pres
Study of DDO 68: nearest candidate for a young galaxy?
We present the results of optical spectroscopy and imaging with the SAO 6m
telescope for the dwarf galaxy DDO 68 (UGC 5340 = VV 542), falling into the
region of very low density of luminous (L > L*) galaxies (Lynx-Cancer void).
Its deep images in V,R bands and in the narrow H-alpha-filter show that the
galaxy has the very irregular morphology, with a long curved tail on the South
and a ring-like structure at the Northern edge. The latter consists of 5
separate regions, in three of which we could measure O/H by the classical T_e
method. Their weighted mean oxygen abundance corresponds to
12+log(O/H)=7.21+-0.03, coincident within uncertainties with those for IZw18.
The (V-R) colour of DDO 68 is rather blue all over the galaxy, indicating the
youth of its stellar populations. Comparing the (V-R)_0 colour of the
underlying exponential disk of 0.12+-0.04 with the PEGASE.2 models for the
evolving stellar clusters, we give the first estimate of the ages of the oldest
stellar population, which needs confirmation by the other colours and the
photometry of resolved stars. These ages are in the range of 200-900 Myr for
continuous star formation law, and 100-115 Myr for the instantaneous starburst.
We discuss the properties and the possible youth of this nearby object (2.3
times closer than the famous young galaxy IZw18) in the context of its atypical
environment.Comment: 13 pages, including 7 tables and 3 postscript figures. Accepted for
publication in Astron.Astrophys. Small language corrections are made after
the A&A Language Edito
ΠΠ½Π°Π»ΠΈΠ· Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎΡΡΠ΅ΠΉ ΠΏΡΠ°ΠΊΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΡ Π³Π°Π·ΠΎΠ²
In recent years, discrete approaches have been widely used in mathematical modeling of physicochemical processes. Cellular automata-based methods greatly simplify modeling procedures in many cases. In particular, this is important when using models in the form of partial differential equations systems to analyze the transfer of a substance in inhomogeneous media. In some cases, it is quite difficult to set the boundary conditions correctly if the object of study has boundaries of complex shape. It is also difficult to use mathematical physics classical equations if one cannot neglect the influence of stochastic effects on the process flow. The lattice gas models considered in the article are one of the types of cellular automata. Until now they have not been widely adopted, despite the fact that the first works on their use appeared about forty years ago. It is known, however, that lattice gases successfully describe a number of hydrodynamic phenomena, and the results obtained do not contradict the generally accepted views on the physical nature of continuous media motion processes. When using models of lattice gases, there are often questions about the correctness of the use of discrete models in various flow regimes. The second problem is a large-scale transition from model discrete parameters to generally accepted macroscopic characteristics of flows, such as flow velocity, viscosity and density of the medium, etc. It is also necessary to take into account that the indicated parameters in the lattice model are dimensionless, and the corresponding real macroscopic parameters have dimension. In this paper, an attempt is made to propose a method of large-scale transition, as well as to indicate the areas of practical use of some models of lattice gases.Π ΠΏΠΎΡΠ»Π΅Π΄Π½ΠΈΠ΅ Π³ΠΎΠ΄Ρ Π΄Π»Ρ ΠΌΠ°ΡΠ΅ΠΌΠ°ΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΌΠΎΠ΄Π΅Π»ΠΈΡΠΎΠ²Π°Π½ΠΈΡ ΡΠΈΠ·ΠΈΠΊΠΎ-Ρ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ² ΡΡΠ°Π»ΠΈ ΡΠΈΡΠΎΠΊΠΎ ΠΏΡΠΈΠΌΠ΅Π½ΡΡΡΡΡ Π΄ΠΈΡΠΊΡΠ΅ΡΠ½ΡΠ΅ ΠΏΠΎΠ΄Ρ
ΠΎΠ΄Ρ. Π‘ΡΠ΅Π΄ΠΈ Π½ΠΈΡ
ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°ΡΠ΅Π»ΠΈ Π²ΡΠ΄Π΅Π»ΡΡΡ ΠΌΠ΅ΡΠΎΠ΄Ρ, ΠΎΡΠ½ΠΎΠ²Π°Π½Π½ΡΠ΅ Π½Π° ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠΈ ΠΊΠ»Π΅ΡΠΎΡΠ½ΡΡ
Π°Π²ΡΠΎΠΌΠ°ΡΠΎΠ². ΠΡΠΈΠ²Π»Π΅ΠΊΠ°ΡΠ΅Π»ΡΠ½ΠΎΡΡΡ Π΄Π°Π½Π½ΡΡ
ΠΌΠ°ΡΠ΅ΠΌΠ°ΡΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΎΠ±ΡΠ΅ΠΊΡΠΎΠ² ΠΎΠ±ΠΎΡΠ½ΠΎΠ²Π°Π½Π° ΠΏΡΠ΅ΠΆΠ΄Π΅ Π²ΡΠ΅Π³ΠΎ ΡΠ΅ΠΌ, ΡΡΠΎ Π²ΠΎ ΠΌΠ½ΠΎΠ³ΠΈΡ
ΡΠ»ΡΡΠ°ΡΡ
ΠΎΠ½ΠΈ ΡΡΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎ ΡΠΏΡΠΎΡΠ°ΡΡ ΠΏΡΠΎΡΠ΅Π΄ΡΡΡ ΠΌΠΎΠ΄Π΅Π»ΠΈΡΠΎΠ²Π°Π½ΠΈΡ ΠΏΠΎ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ Ρ ΡΡΠ°Π΄ΠΈΡΠΈΠΎΠ½Π½ΡΠΌΠΈ ΠΌΠ΅ΡΠΎΠ΄Π°ΠΌΠΈ. Π ΡΠ°ΡΡΠ½ΠΎΡΡΠΈ, ΠΏΡΠΈ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠΈ ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ Π² Π²ΠΈΠ΄Π΅ ΡΠΈΡΡΠ΅ΠΌ Π΄ΠΈΡΡΠ΅ΡΠ΅Π½ΡΠΈΠ°Π»ΡΠ½ΡΡ
ΡΡΠ°Π²Π½Π΅Π½ΠΈΠΉ Ρ ΡΠ°ΡΡΠ½ΡΠΌΠΈ ΠΏΡΠΎΠΈΠ·Π²ΠΎΠ΄Π½ΡΠΌΠΈ Π΄Π»Ρ Π°Π½Π°Π»ΠΈΠ·Π° ΠΏΠ΅ΡΠ΅Π½ΠΎΡΠ° ΡΡΠ±ΡΡΠ°Π½ΡΠΈΠΈ, ΡΡΡΠ΄Π½ΠΎΡΡΠΈ Π²ΠΎΠ·Π½ΠΈΠΊΠ°ΡΡ Π² ΡΠ»ΡΡΠ°ΡΡ
ΠΏΡΠΎΡΠ΅ΠΊΠ°Π½ΠΈΡ ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ² Π² Π½Π΅ΠΎΠ΄Π½ΠΎΡΠΎΠ΄Π½ΡΡ
ΡΡΠ΅Π΄Π°Ρ
. ΠΡΠΎΠΌΠ΅ ΡΠΎΠ³ΠΎ, Π² ΡΡΠ΄Π΅ ΡΠ»ΡΡΠ°Π΅Π² Π΄ΠΎΠ²ΠΎΠ»ΡΠ½ΠΎ ΠΏΡΠΎΠ±Π»Π΅ΠΌΠ°ΡΠΈΡΠ½ΠΎ ΠΎΡΡΡΠ΅ΡΡΠ²ΠΈΡΡ ΠΊΠΎΡΡΠ΅ΠΊΡΠ½ΡΡ ΠΏΠΎΡΡΠ°Π½ΠΎΠ²ΠΊΡ Π³ΡΠ°Π½ΠΈΡΠ½ΡΡ
ΡΡΠ»ΠΎΠ²ΠΈΠΉ, Π΅ΡΠ»ΠΈ ΠΎΠ±ΡΠ΅ΠΊΡ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΠΈΠΌΠ΅Π΅Ρ Π³ΡΠ°Π½ΠΈΡΡ ΡΠ»ΠΎΠΆΠ½ΠΎΠΉ ΡΠΎΡΠΌΡ. Π’Π°ΠΊΠΆΠ΅ ΡΡΡΠ΄Π½ΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°ΡΡ ΠΊΠ»Π°ΡΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ ΠΌΠ°ΡΠ΅ΠΌΠ°ΡΠΈΡΠ΅ΡΠΊΠΎΠΉ ΡΠΈΠ·ΠΈΠΊΠΈ Π² ΡΡΠ»ΠΎΠ²ΠΈΡΡ
, ΠΊΠΎΠ³Π΄Π° Π½Π΅Π²ΠΎΠ·ΠΌΠΎΠΆΠ½ΠΎ ΠΈΠ³Π½ΠΎΡΠΈΡΠΎΠ²Π°ΡΡ Π²Π»ΠΈΡΠ½ΠΈΠΈ ΡΡΠΎΡ
Π°ΡΡΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΡΡΠ΅ΠΊΡΠΎΠ² Π½Π° ΠΏΡΠΎΡΠ΅ΠΊΠ°Π½ΠΈΠ΅ ΠΏΡΠΎΡΠ΅ΡΡΠ°. ΠΠΈΡΠΊΡΠ΅ΡΠ½ΡΠ΅ ΠΏΠΎΠ΄Ρ
ΠΎΠ΄Ρ Π² Π·Π½Π°ΡΠΈΡΠ΅Π»ΡΠ½ΠΎΠΉ ΠΌΠ΅ΡΠ΅ ΡΠ²ΠΎΠ±ΠΎΠ΄Π½Ρ ΠΎΡ ΡΠΊΠ°Π·Π°Π½Π½ΡΡ
Π½Π΅Π΄ΠΎΡΡΠ°ΡΠΊΠΎΠ². Π Π°ΡΡΠΌΠ°ΡΡΠΈΠ²Π°Π΅ΠΌΡΠ΅ Π² ΡΡΠ°ΡΡΠ΅ ΠΌΠΎΠ΄Π΅Π»ΠΈ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΡ
Π³Π°Π·ΠΎΠ² ΡΠ²Π»ΡΡΡΡΡ ΠΎΠ΄Π½ΠΎΠΉ ΠΈΠ· ΡΠ°Π·Π½ΠΎΠ²ΠΈΠ΄Π½ΠΎΡΡΠ΅ΠΉ ΠΊΠ»Π΅ΡΠΎΡΠ½ΡΡ
Π°Π²ΡΠΎΠΌΠ°ΡΠΎΠ². ΠΠ΅ΡΠΌΠΎΡΡΡ Π½Π° ΡΠΎ, ΡΡΠΎ ΠΏΠ΅ΡΠ²ΡΠ΅ ΡΠ°Π±ΠΎΡΡ ΠΏΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΡ
ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ Π³Π°Π·ΠΎΠ² ΠΏΠΎΡΠ²ΠΈΠ»ΠΈΡΡ ΠΎΠΊΠΎΠ»ΠΎ ΡΠΎΡΠΎΠΊΠ° Π»Π΅Ρ Π½Π°Π·Π°Π΄, ΠΎΠ½ΠΈ Π΄ΠΎ Π½Π°ΡΡΠΎΡΡΠ΅Π³ΠΎ Π²ΡΠ΅ΠΌΠ΅Π½ΠΈ Π½Π΅ ΠΏΠΎΠ»ΡΡΠΈΠ»ΠΈ ΡΠΈΡΠΎΠΊΠΎΠ³ΠΎ ΡΠ°ΡΠΏΡΠΎΡΡΡΠ°Π½Π΅Π½ΠΈΡ Π² ΡΡΠ΅Π΄Π΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°ΡΠ΅Π»Π΅ΠΉ Π΅ΡΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ½Π°ΡΡΠ½ΡΡ
ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ². Π’Π΅ΠΌ Π½Π΅ ΠΌΠ΅Π½Π΅Π΅ ΠΈΠΌΠ΅Π΅ΡΡΡ ΠΌΠ½ΠΎΠ³ΠΎ Π΄ΠΎΠΊΠ°Π·Π°ΡΠ΅Π»ΡΡΡΠ² ΡΠΎΠ³ΠΎ, ΡΡΠΎ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΠ΅ Π³Π°Π·Ρ Π΄ΠΎΡΡΠ°ΡΠΎΡΠ½ΠΎ ΡΡΠΏΠ΅ΡΠ½ΠΎ ΠΎΠΏΠΈΡΡΠ²Π°ΡΡ ΡΠ΅Π»ΡΠΉ ΡΡΠ΄ Π³ΠΈΠ΄ΡΠΎΠ΄ΠΈΠ½Π°ΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΠ²Π»Π΅Π½ΠΈΠΉ, Π° ΠΏΠΎΠ»ΡΡΠ΅Π½Π½ΡΠ΅ ΡΠ΅Π·ΡΠ»ΡΡΠ°ΡΡ Π½Π΅ ΠΏΡΠΎΡΠΈΠ²ΠΎΡΠ΅ΡΠ°Ρ ΠΎΠ±ΡΠ΅ΠΏΡΠΈΠ½ΡΡΡΠΌ Π²Π·Π³Π»ΡΠ΄Π°ΠΌ Π½Π° ΡΠΈΠ·ΠΈΡΠ΅ΡΠΊΡΡ ΠΏΡΠΈΡΠΎΠ΄Ρ ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ² Π΄Π²ΠΈΠΆΠ΅Π½ΠΈΡ ΡΠΏΠ»ΠΎΡΠ½ΡΡ
ΡΡΠ΅Π΄. ΠΠ΅ΡΠΌΠΎΡΡΡ Π½Π° ΠΏΠΎΡΠ²Π»Π΅Π½ΠΈΠ΅ Π·Π½Π°ΡΠΈΡΠ΅Π»ΡΠ½ΠΎΠ³ΠΎ ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π° ΡΠ°Π·Π½ΠΎΠ²ΠΈΠ΄Π½ΠΎΡΡΠ΅ΠΉ ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΡ
Π³Π°Π·ΠΎΠ², ΠΏΡΠΈ ΠΈΡ
ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠΈ ΡΠ°ΡΡΠΎ Π²ΠΎΠ·Π½ΠΈΠΊΠ°ΡΡ Π²ΠΎΠΏΡΠΎΡΡ, ΠΊΠ°ΡΠ°ΡΡΠΈΠ΅ΡΡ ΡΠ΅ΠΆΠΈΠΌΠΎΠ² ΡΠ΅ΡΠ΅Π½ΠΈΡ, ΠΏΡΠΈ ΠΊΠΎΡΠΎΡΡΡ
ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ Π΄ΠΈΡΠΊΡΠ΅ΡΠ½ΡΡ
ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ Π±ΡΠ΄Π΅Ρ ΠΊΠΎΡΡΠ΅ΠΊΡΠ½ΡΠΌ. ΠΡΠΎΡΠ°Ρ ΠΏΡΠΎΠ±Π»Π΅ΠΌΠ°, ΠΎΠ±ΡΡΠ½ΠΎ Π²ΠΎΠ·Π½ΠΈΠΊΠ°ΡΡΠ°Ρ ΠΏΠ΅ΡΠ΅Π΄ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°ΡΠ΅Π»ΡΠΌΠΈ, ΠΈΡΠΏΠΎΠ»ΡΠ·ΡΡΡΠΈΠΌΠΈ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΠ΅ ΠΌΠΎΠ΄Π΅Π»ΠΈ, - ΡΡΠΎ ΠΌΠ°ΡΡΡΠ°Π±Π½ΡΠΉ ΠΏΠ΅ΡΠ΅Ρ
ΠΎΠ΄ ΠΎΡ ΠΌΠΎΠ΄Π΅Π»ΡΠ½ΡΡ
Π΄ΠΈΡΠΊΡΠ΅ΡΠ½ΡΡ
ΠΏΠ°ΡΠ°ΠΌΠ΅ΡΡΠΎΠ² ΠΊ ΠΎΠ±ΡΠ΅ΠΏΡΠΈΠ½ΡΡΡΠΌ ΠΌΠ°ΠΊΡΠΎΡΠΊΠΎΠΏΠΈΡΠ΅ΡΠΊΠΈΠΌ Ρ
Π°ΡΠ°ΠΊΡΠ΅ΡΠΈΡΡΠΈΠΊΠ°ΠΌ ΡΠ΅ΡΠ΅Π½ΠΈΠΉ. ΠΠ΄Π΅ΡΡ, ΠΏΡΠ΅ΠΆΠ΄Π΅ Π²ΡΠ΅Π³ΠΎ, ΠΈΠΌΠ΅ΡΡΡΡ Π² Π²ΠΈΠ΄Ρ ΡΠ°ΠΊΠΈΠ΅ ΡΠΈΠ·ΠΈΡΠ΅ΡΠΊΠΈΠ΅ Π²Π΅Π»ΠΈΡΠΈΠ½Ρ, ΠΊΠ°ΠΊ ΡΠΊΠΎΡΠΎΡΡΡ ΠΏΠΎΡΠΎΠΊΠ°, Π²ΡΠ·ΠΊΠΎΡΡΡ ΠΈ ΠΏΠ»ΠΎΡΠ½ΠΎΡΡΡ ΡΡΠ΅Π΄Ρ ΠΈ ΠΏΡ. Π‘ΠΈΡΡΠ°ΡΠΈΡ ΠΎΡΠ»ΠΎΠΆΠ½ΡΠ΅ΡΡΡ ΡΠ΅ΠΌ ΠΎΠ±ΡΡΠΎΡΡΠ΅Π»ΡΡΡΠ²ΠΎΠΌ, ΡΡΠΎ ΡΠΊΠ°Π·Π°Π½Π½ΡΠ΅ ΠΏΠ°ΡΠ°ΠΌΠ΅ΡΡΡ Π² ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΠΎΠΉ ΠΌΠΎΠ΄Π΅Π»ΠΈ ΡΠ²Π»ΡΡΡΡΡ Π±Π΅Π·ΡΠ°Π·ΠΌΠ΅ΡΠ½ΡΠΌΠΈ, Π° ΡΠΎΠΎΡΠ²Π΅ΡΡΡΠ²ΡΡΡΠΈΠ΅ ΡΠ΅Π°Π»ΡΠ½ΡΠ΅ ΠΌΠ°ΠΊΡΠΎΡΠΊΠΎΠΏΠΈΡΠ΅ΡΠΊΠΈΠ΅ ΠΏΠΎΠΊΠ°Π·Π°ΡΠ΅Π»ΠΈ ΠΈΠΌΠ΅ΡΡ ΡΠ°Π·ΠΌΠ΅ΡΠ½ΠΎΡΡΡ. Π Π΄Π°Π½Π½ΠΎΠΉ ΡΡΠ°ΡΡΠ΅ Π΄Π΅Π»Π°Π΅ΡΡΡ ΠΏΠΎΠΏΡΡΠΊΠ° ΠΏΡΠ΅Π΄Π»ΠΎΠΆΠΈΡΡ ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊΡ ΠΌΠ°ΡΡΡΠ°Π±Π½ΠΎΠ³ΠΎ ΠΏΠ΅ΡΠ΅Ρ
ΠΎΠ΄Π°, Π° ΡΠ°ΠΊΠΆΠ΅ ΡΠΊΠ°Π·Π°ΡΡ ΠΎΠ±Π»Π°ΡΡΠΈ ΠΏΡΠ°ΠΊΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ Π½Π΅ΠΊΠΎΡΠΎΡΡΡ
ΠΌΠΎΠ΄Π΅Π»Π΅ΠΉ ΡΠ΅ΡΠ΅ΡΠΎΡΠ½ΡΡ
Π³Π°Π·ΠΎΠ²
Π‘Π ΠΠΠΠΠ’ΠΠΠ¬ΠΠ«Π ΠΠΠΠΠΠ ΠΠΠ’ΠΠΠΠ Π ΠΠΠ’ΠΠΠΠΠ€ΠΠ£ΠΠ ΠΠ‘Π¦ΠΠΠ’ΠΠΠΠ ΠΠΠ ΠΠΠΠΠΠΠΠ― ΠΠΠΠΠΠΠ’ΠΠΠΠ Π‘ΠΠ‘Π’ΠΠΠ ΠΠ Π₯ΠΠΠΠΠΠΠ§ΠΠ‘ΠΠΠ ΠΠΠ ΠΠΠΠΠ ΠΠ ΠΠΠΠ«Π₯ ΠΠΠΠΠ‘ΠΠ
Wavelength-dispersive X-ray fluorescence analysis (WDXRF) and total-reflection X-ray fluorescence (TXRF) analysis were applied to study the elemental composition of the Late Neolithic ancient ceramics collected at the Popovsky Lug burial site (Kachug, Upper Lena river, Russia). Semi-quantitative non-destructive analysis of ceramic pieces showed that measurements of the upper and lower sides of the ceramic are less informative than the measurement of its cut. Various sample preparation techniques for the low quantity of crushed ceramics such as fusion, pressing and preparation of suspensions were compared to preserve the material. Samples were prepared as 150 mg fused beads and 250 mg pressed pellets for WDXRF, and as suspensions of 20 mg sample based on the aqueous solution of the Triton X-100 surfactant for TXRF. Certified methods were used to validate the obtained contents of rock-forming oxides and inductively coupled plasma mass spectrometry was used to confirm the results of trace elements determination. Based on the carried-out studies, a combination of the wavelength-dispersive X-ray fluorescence analysis (glass) and total-reflection X-ray fluorescence analysis (suspension) methods was chosen to obtain the data on the elemental bulk composition of archaeological ceramics. The proposed combination allowed the quantitative determination of Na, Mg, Al, Si, P, K, Ca, Ti, Mn, Fe, V, Cr, Ni, Cu, Zn, Ga, Rb, Sr, Y, Zr, Pb, and Ba from the sample of crushed ceramics weighing only about 170 mg.Keywords: wavelength-dispersive X-ray fluorescence analysis, total reflection X-ray fluorescence analysis, ceramics, archeology, Popovsky Lug, Upper Lena RiverΒ DOI: http://dx.doi.org/10.15826/analitika.2020.25.1.001Β G.V. Pashkova1,2, M.M. Mukhamedova1,2, V.M. Chubarov1,3, A.S. Maltsev1,4,A.A. Amosova3, E.I. Demonterova1, E.A. Mikheeva1, D.L. Shergin1,2,5, V.A. Pellinen1, A.V. Teten'kin1,4Β 1Institute of the Eatrhβs Crust, SB RAS, 128 Lermontov St., 640033, Irkutsk, Russian Federation2Irkutsk State University, 1 K. Marx St., 664003, Irkutsk, Russian Federation3Vinogradov Institute of Geochemistry, SB RAS, 1Π Favorsky st., 664033, Irkutsk, Russian Federation4Irkutsk National Research Technical University, 83 Lermontov st., 664074, Irkutsk, Russian Federation5Irkutsk Regional Museum of Local Lore; 13 K. Marx st., 664003, Irkutsk, Russian FederationΠΠ»Ρ ΠΈΠ·ΡΡΠ΅Π½ΠΈΡ ΡΠ»Π΅ΠΌΠ΅Π½ΡΠ½ΠΎΠ³ΠΎ ΡΠΎΡΡΠ°Π²Π° Π΄ΡΠ΅Π²Π½Π΅ΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΡΠΏΠΎΡ
ΠΈ ΠΏΠΎΠ·Π΄Π½Π΅Π³ΠΎ Π½Π΅ΠΎΠ»ΠΈΡΠ° ΡΡΠΎΡΠ½ΠΊΠΈ-ΠΌΠΎΠ³ΠΈΠ»ΡΠ½ΠΈΠΊΠ° ΠΠΎΠΏΠΎΠ²ΡΠΊΠΈΠΉ ΠΡΠ³ (ΡΠ°ΠΉΠΎΠ½ ΠΏΠΎΡΠ΅Π»ΠΊΠ° ΠΠ°ΡΡΠ³, Π²Π΅ΡΡ
ΠΎΠ²ΡΠ΅ ΡΠ΅ΠΊΠΈ ΠΠ΅Π½Ρ, Π ΠΎΡΡΠΈΡ) ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½Ρ Π΄Π²Π° Π²Π°ΡΠΈΠ°Π½ΡΠ° ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΠΎΠ³ΠΎ Π°Π½Π°Π»ΠΈΠ·Π°: ΡΡΠ°Π΄ΠΈΡΠΈΠΎΠ½Π½ΡΠΉ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ Π²ΠΎΠ»Π½ΠΎΠ²ΠΎΠΉ Π΄ΠΈΡΠΏΠ΅ΡΡΠΈΠ΅ΠΉ (WDXRF) ΠΈ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ ΠΏΠΎΠ»Π½ΡΠΌ Π²Π½Π΅ΡΠ½ΠΈΠΌ ΠΎΡΡΠ°ΠΆΠ΅Π½ΠΈΠ΅ΠΌ (TXRF). ΠΡΠΈΠ±Π»ΠΈΠΆΠ΅Π½Π½ΠΎ-ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· ΡΡΠ°Π³ΠΌΠ΅Π½ΡΠΎΠ² ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ Π±Π΅Π· ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½ΠΈΡ ΠΏΠΎΠΊΠ°Π·Π°Π», ΡΡΠΎ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΡ Π²Π½Π΅ΡΠ½Π΅ΠΉ ΠΈ Π²Π½ΡΡΡΠ΅Π½Π½Π΅ΠΉ ΠΏΠΎΠ²Π΅ΡΡ
Π½ΠΎΡΡΠΈ ΡΡΠ°Π³ΠΌΠ΅Π½ΡΠΎΠ² ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΡΠ²Π»ΡΡΡΡΡ ΠΌΠ΅Π½Π΅Π΅ ΠΈΠ½ΡΠΎΡΠΌΠ°ΡΠΈΠ²Π½ΡΠΌΠΈ, ΠΏΠΎ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ Ρ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΠ΅ΠΌ Π΅Π΅ ΡΡΠ΅Π·Π°. ΠΠΏΡΠΎΠ±ΠΈΡΠΎΠ²Π°Π½Ρ ΡΠΏΠΎΡΠΎΠ±Ρ ΠΏΠΎΠ΄Π³ΠΎΡΠΎΠ²ΠΊΠΈ ΠΏΡΠΎΠ±, ΠΎΡΠΈΠ΅Π½ΡΠΈΡΠΎΠ²Π°Π½Π½ΡΠ΅ Π½Π° Π°Π½Π°Π»ΠΈΠ· ΠΌΠ°Π»ΡΡ
Π½Π°Π²Π΅ΡΠΎΠΊ ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½Π½ΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ Ρ ΡΠ΅Π»ΡΡ ΡΠΎΡ
ΡΠ°Π½Π΅Π½ΠΈΡ ΠΌΠ°ΡΠ΅ΡΠΈΠ°Π»Π°: ΡΠΏΠ»Π°Π²Π»Π΅Π½ΠΈΠ΅, ΠΏΡΠ΅ΡΡΠΎΠ²Π°Π½ΠΈΠ΅ ΠΈ ΠΏΡΠΈΠ³ΠΎΡΠΎΠ²Π»Π΅Π½ΠΈΠ΅ ΡΡΡΠΏΠ΅Π½Π·ΠΈΠΉ. ΠΠ»Ρ WDXRF ΠΈΠ·Π»ΡΡΠ°ΡΠ΅Π»ΠΈ Π³ΠΎΡΠΎΠ²ΠΈΠ»ΠΈ Π² Π²ΠΈΠ΄Π΅ ΡΠΏΠ»Π°Π²Π»Π΅Π½Π½ΡΡ
ΡΡΠ΅ΠΊΠΎΠ» ΠΈΠ· 150 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ, Π° ΡΠ°ΠΊΠΆΠ΅ Π² Π²ΠΈΠ΄Π΅ ΠΏΡΠ΅ΡΡΠΎΠ²Π°Π½Π½ΡΡ
ΡΠ°Π±Π»Π΅ΡΠΎΠΊ ΠΈΠ· 250 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ. ΠΠ»Ρ ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ TXRF ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π»ΠΈ ΡΡΡΠΏΠ΅Π½Π·ΠΈΠΈ ΠΈΠ· 20 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ Π²ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΡΠ°ΡΡΠ²ΠΎΡΠ° ΠΏΠΎΠ²Π΅ΡΡ
Π½ΠΎΡΡΠ½ΠΎ-Π°ΠΊΡΠΈΠ²Π½ΠΎΠ³ΠΎ Π²Π΅ΡΠ΅ΡΡΠ²Π° Triton X-100. Π ΠΊΠ°ΡΠ΅ΡΡΠ²Π΅ ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ ΠΏΡΠΈ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠΈ ΠΏΠΎΡΠΎΠ΄ΠΎΠΎΠ±ΡΠ°Π·ΡΡΡΠΈΡ
ΠΎΠΊΡΠΈΠ΄ΠΎΠ² ΠΏΡΠΈΠΌΠ΅Π½ΡΠ»ΠΈ Π°ΡΡΠ΅ΡΡΠΎΠ²Π°Π½Π½ΡΠ΅ ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊΠΈ ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ³ΠΎ Ρ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ Π°Π½Π°Π»ΠΈΠ·Π°, ΠΏΡΠΈ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠΈ ΠΌΠΈΠΊΡΠΎΡΠ»Π΅ΠΌΠ΅Π½ΡΠΎΠ² β ΠΌΠ΅ΡΠΎΠ΄ ΠΌΠ°ΡΡ-ΡΠΏΠ΅ΠΊΡΡΠΎΠΌΠ΅ΡΡΠΈΠΈ Ρ ΠΈΠ½Π΄ΡΠΊΡΠΈΠ²Π½ΠΎ-ΡΠ²ΡΠ·Π°Π½Π½ΠΎΠΉ ΠΏΠ»Π°Π·ΠΌΠΎΠΉ. ΠΡΠΎΠ²Π΅Π΄Π΅Π½Π½ΡΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΠΏΠΎΠΊΠ°Π·Π°Π»ΠΈ, ΡΡΠΎ Π΄Π»Ρ ΠΏΠΎΠ»ΡΡΠ΅Π½ΠΈΡ Π΄Π°Π½Π½ΡΡ
ΠΎΠ± ΡΠ»Π΅ΠΌΠ΅Π½ΡΠ½ΠΎΠΌ Π²Π°Π»ΠΎΠ²ΠΎΠΌ ΡΠΎΡΡΠ°Π²Π΅ Π°ΡΡ
Π΅ΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΠΏΡΠ΅Π΄ΠΏΠΎΡΡΠΈΡΠ΅Π»ΡΠ½ΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ ΠΊΠΎΠΌΠ±ΠΈΠ½Π°ΡΠΈΠΈ ΠΌΠ΅ΡΠΎΠ΄ΠΎΠ² WDXRF (ΡΡΠ΅ΠΊΠ»ΠΎ) ΠΈ TXRF (ΡΡΡΠΏΠ΅Π½Π·ΠΈΡ). ΠΡΠ΅Π΄Π»ΠΎΠΆΠ΅Π½Π½Π°Ρ ΡΡ
Π΅ΠΌΠ° ΠΏΠΎΠ·Π²ΠΎΠ»ΡΠ΅Ρ ΠΏΡΠΎΠ²ΠΎΠ΄ΠΈΡΡ ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ΅ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠ΅ Na, Mg, Al, Si, P, K, Ca, Ti, Mn, Fe, V, Cr, Ni, Cu, Zn, Ga, Rb, Sr, Y, Zr, Pb ΠΈ Ba ΠΈΠ· Π½Π°Π²Π΅ΡΠΊΠΈ ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½Π½ΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΠΌΠ°ΡΡΠΎΠΉ ΠΏΡΠΈΠΌΠ΅ΡΠ½ΠΎ 170 ΠΌΠ³.ΠΠ»ΡΡΠ΅Π²ΡΠ΅ ΡΠ»ΠΎΠ²Π°: ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ Π²ΠΎΠ»Π½ΠΎΠ²ΠΎΠΉ Π΄ΠΈΡΠΏΠ΅ΡΡΠΈΠ΅ΠΉ, ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ ΠΏΠΎΠ»Π½ΡΠΌ Π²Π½Π΅ΡΠ½ΠΈΠΌ ΠΎΡΡΠ°ΠΆΠ΅Π½ΠΈΠ΅ΠΌ, ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠ°, Π°ΡΡ
Π΅ΠΎΠ»ΠΎΠ³ΠΈΡ, ΠΠΎΠΏΠΎΠ²ΡΠΊΠΈΠΉ ΠΡΠ³, ΠΠ΅ΡΡ
Π½ΡΡ ΠΠ΅Π½Π°DOI: http://dx.doi.org/10.15826/analitika.2020.25.1.00
Comparative analysis of X-ray fluorescence methods for elemental composition determination of the archaeological ceramics from low sample quantity
ΠΠ»Ρ ΠΈΠ·ΡΡΠ΅Π½ΠΈΡ ΡΠ»Π΅ΠΌΠ΅Π½ΡΠ½ΠΎΠ³ΠΎ ΡΠΎΡΡΠ°Π²Π° Π΄ΡΠ΅Π²Π½Π΅ΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΡΠΏΠΎΡ
ΠΈ ΠΏΠΎΠ·Π΄Π½Π΅Π³ΠΎ Π½Π΅ΠΎΠ»ΠΈΡΠ° ΡΡΠΎΡΠ½ΠΊΠΈ-ΠΌΠΎΠ³ΠΈΠ»ΡΠ½ΠΈΠΊΠ° ΠΠΎΠΏΠΎΠ²ΡΠΊΠΈΠΉ ΠΡΠ³ (ΡΠ°ΠΉΠΎΠ½ ΠΏΠΎΡΠ΅Π»ΠΊΠ° ΠΠ°ΡΡΠ³, Π²Π΅ΡΡ
ΠΎΠ²ΡΠ΅ ΡΠ΅ΠΊΠΈ ΠΠ΅Π½Ρ, Π ΠΎΡΡΠΈΡ) ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½Ρ Π΄Π²Π° Π²Π°ΡΠΈΠ°Π½ΡΠ° ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΠΎΠ³ΠΎ Π°Π½Π°Π»ΠΈΠ·Π°: ΡΡΠ°Π΄ΠΈΡΠΈΠΎΠ½Π½ΡΠΉ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ Π²ΠΎΠ»Π½ΠΎΠ²ΠΎΠΉ Π΄ΠΈΡΠΏΠ΅ΡΡΠΈΠ΅ΠΉ (WDXRF) ΠΈ ΡΠ΅Π½ΡΠ³Π΅Π½ΠΎΡΠ»ΡΠΎΡΠ΅ΡΡΠ΅Π½ΡΠ½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· Ρ ΠΏΠΎΠ»Π½ΡΠΌ Π²Π½Π΅ΡΠ½ΠΈΠΌ ΠΎΡΡΠ°ΠΆΠ΅Π½ΠΈΠ΅ΠΌ (TXRF). ΠΡΠΈΠ±Π»ΠΈΠΆΠ΅Π½Π½ΠΎ-ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΡΠΉ Π°Π½Π°Π»ΠΈΠ· ΡΡΠ°Π³ΠΌΠ΅Π½ΡΠΎΠ² ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ Π±Π΅Π· ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½ΠΈΡ ΠΏΠΎΠΊΠ°Π·Π°Π», ΡΡΠΎ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΡ Π²Π½Π΅ΡΠ½Π΅ΠΉ ΠΈ Π²Π½ΡΡΡΠ΅Π½Π½Π΅ΠΉ ΠΏΠΎΠ²Π΅ΡΡ
Π½ΠΎΡΡΠΈ ΡΡΠ°Π³ΠΌΠ΅Π½ΡΠΎΠ² ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΡΠ²Π»ΡΡΡΡΡ ΠΌΠ΅Π½Π΅Π΅ ΠΈΠ½ΡΠΎΡΠΌΠ°ΡΠΈΠ²Π½ΡΠΌΠΈ, ΠΏΠΎ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ Ρ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΠ΅ΠΌ Π΅Π΅ ΡΡΠ΅Π·Π°. ΠΠΏΡΠΎΠ±ΠΈΡΠΎΠ²Π°Π½Ρ ΡΠΏΠΎΡΠΎΠ±Ρ ΠΏΠΎΠ΄Π³ΠΎΡΠΎΠ²ΠΊΠΈ ΠΏΡΠΎΠ±, ΠΎΡΠΈΠ΅Π½ΡΠΈΡΠΎΠ²Π°Π½Π½ΡΠ΅ Π½Π° Π°Π½Π°Π»ΠΈΠ· ΠΌΠ°Π»ΡΡ
Π½Π°Π²Π΅ΡΠΎΠΊ ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½Π½ΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ Ρ ΡΠ΅Π»ΡΡ ΡΠΎΡ
ΡΠ°Π½Π΅Π½ΠΈΡ ΠΌΠ°ΡΠ΅ΡΠΈΠ°Π»Π°: ΡΠΏΠ»Π°Π²Π»Π΅Π½ΠΈΠ΅, ΠΏΡΠ΅ΡΡΠΎΠ²Π°Π½ΠΈΠ΅ ΠΈ ΠΏΡΠΈΠ³ΠΎΡΠΎΠ²Π»Π΅Π½ΠΈΠ΅ ΡΡΡΠΏΠ΅Π½Π·ΠΈΠΉ. ΠΠ»Ρ WDXRF ΠΈΠ·Π»ΡΡΠ°ΡΠ΅Π»ΠΈ Π³ΠΎΡΠΎΠ²ΠΈΠ»ΠΈ Π² Π²ΠΈΠ΄Π΅ ΡΠΏΠ»Π°Π²Π»Π΅Π½Π½ΡΡ
ΡΡΠ΅ΠΊΠΎΠ» ΠΈΠ· 150 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ, Π° ΡΠ°ΠΊΠΆΠ΅ Π² Π²ΠΈΠ΄Π΅ ΠΏΡΠ΅ΡΡΠΎΠ²Π°Π½Π½ΡΡ
ΡΠ°Π±Π»Π΅ΡΠΎΠΊ ΠΈΠ· 250 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ. ΠΠ»Ρ ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ TXRF ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π»ΠΈ ΡΡΡΠΏΠ΅Π½Π·ΠΈΠΈ ΠΈΠ· 20 ΠΌΠ³ ΠΏΡΠΎΠ±Ρ Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ Π²ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΡΠ°ΡΡΠ²ΠΎΡΠ° ΠΏΠΎΠ²Π΅ΡΡ
Π½ΠΎΡΡΠ½ΠΎ-Π°ΠΊΡΠΈΠ²Π½ΠΎΠ³ΠΎ Π²Π΅ΡΠ΅ΡΡΠ²Π° Triton X-100. Π ΠΊΠ°ΡΠ΅ΡΡΠ²Π΅ ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊ ΡΡΠ°Π²Π½Π΅Π½ΠΈΡ ΠΏΡΠΈ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠΈ ΠΏΠΎΡΠΎΠ΄ΠΎΠΎΠ±ΡΠ°Π·ΡΡΡΠΈΡ
ΠΎΠΊΡΠΈΠ΄ΠΎΠ² ΠΏΡΠΈΠΌΠ΅Π½ΡΠ»ΠΈ Π°ΡΡΠ΅ΡΡΠΎΠ²Π°Π½Π½ΡΠ΅ ΠΌΠ΅ΡΠΎΠ΄ΠΈΠΊΠΈ ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ³ΠΎ Ρ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ Π°Π½Π°Π»ΠΈΠ·Π°, ΠΏΡΠΈ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠΈ ΠΌΠΈΠΊΡΠΎΡΠ»Π΅ΠΌΠ΅Π½ΡΠΎΠ² β ΠΌΠ΅ΡΠΎΠ΄ ΠΌΠ°ΡΡ-ΡΠΏΠ΅ΠΊΡΡΠΎΠΌΠ΅ΡΡΠΈΠΈ Ρ ΠΈΠ½Π΄ΡΠΊΡΠΈΠ²Π½ΠΎ-ΡΠ²ΡΠ·Π°Π½Π½ΠΎΠΉ ΠΏΠ»Π°Π·ΠΌΠΎΠΉ. ΠΡΠΎΠ²Π΅Π΄Π΅Π½Π½ΡΠ΅ ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΠΏΠΎΠΊΠ°Π·Π°Π»ΠΈ, ΡΡΠΎ Π΄Π»Ρ ΠΏΠΎΠ»ΡΡΠ΅Π½ΠΈΡ Π΄Π°Π½Π½ΡΡ
ΠΎΠ± ΡΠ»Π΅ΠΌΠ΅Π½ΡΠ½ΠΎΠΌ Π²Π°Π»ΠΎΠ²ΠΎΠΌ ΡΠΎΡΡΠ°Π²Π΅ Π°ΡΡ
Π΅ΠΎΠ»ΠΎΠ³ΠΈΡΠ΅ΡΠΊΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΠΏΡΠ΅Π΄ΠΏΠΎΡΡΠΈΡΠ΅Π»ΡΠ½ΠΎ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ ΠΊΠΎΠΌΠ±ΠΈΠ½Π°ΡΠΈΠΈ ΠΌΠ΅ΡΠΎΠ΄ΠΎΠ² WDXRF (ΡΡΠ΅ΠΊΠ»ΠΎ) ΠΈ TXRF (ΡΡΡΠΏΠ΅Π½Π·ΠΈΡ). ΠΡΠ΅Π΄Π»ΠΎΠΆΠ΅Π½Π½Π°Ρ ΡΡ
Π΅ΠΌΠ° ΠΏΠΎΠ·Π²ΠΎΠ»ΡΠ΅Ρ ΠΏΡΠΎΠ²ΠΎΠ΄ΠΈΡΡ ΠΊΠΎΠ»ΠΈΡΠ΅ΡΡΠ²Π΅Π½Π½ΠΎΠ΅ ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠ΅ Na, Mg, Al, Si, P, K, Ca, Ti, Mn, Fe, V, Cr, Ni, Cu, Zn, Ga, Rb, Sr, Y, Zr, Pb ΠΈ Ba ΠΈΠ· Π½Π°Π²Π΅ΡΠΊΠΈ ΠΈΠ·ΠΌΠ΅Π»ΡΡΠ΅Π½Π½ΠΎΠΉ ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΠΌΠ°ΡΡΠΎΠΉ ΠΏΡΠΈΠΌΠ΅ΡΠ½ΠΎ 170 ΠΌΠ³.Wavelength-dispersive X-ray fluorescence analysis (WDXRF) and total-reflection X-ray fluorescence (TXRF) analysis were applied to study the elemental composition of the Late Neolithic ancient ceramics collected at the Popovsky Lug burial site (Kachug, Upper Lena river, Russia). Semi-quantitative non-destructive analysis of ceramic pieces showed that measurements of the upper and lower sides of the ceramic are less informative than the measurement of its cut. Various sample preparation techniques for the low quantity of crushed ceramics such as fusion, pressing and preparation of suspensions were compared to preserve the material. Samples were prepared as 150 mg fused beads and 250 mg pressed pellets for WDXRF, and as suspensions of 20 mg sample based on the aqueous solution of the Triton X-100 surfactant for TXRF. Certified methods were used to validate the obtained contents of rock-forming oxides and inductively coupled plasma mass spectrometry was used to confirm the results of trace elements determination. Based on the carried-out studies, a combination of the wavelength-dispersive X-ray fluorescence analysis (glass) and total-reflection X-ray fluorescence analysis (suspension) methods was chosen to obtain the data on the elemental bulk composition of archaeological ceramics. The proposed combination allowed the quantitative determination of Na, Mg, Al, Si, P, K, Ca, Ti, Mn, Fe, V, Cr, Ni, Cu, Zn, Ga, Rb, Sr, Y, Zr, Pb, and Ba from the sample of crushed ceramics weighing only about 170 mg.Π Π°Π±ΠΎΡΠ° Π²ΡΠΏΠΎΠ»Π½Π΅Π½Π° ΠΏΡΠΈ ΡΠΈΠ½Π°Π½ΡΠΎΠ²ΠΎΠΉ ΠΏΠΎΠ΄Π΄Π΅ΡΠΆΠΊΠ΅ Π³ΡΠ°Π½ΡΠ° Π ΠΠ€ β 19-78-10084. ΠΡΠ΅ ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΡ ΠΏΡΠΎΠ²ΠΎΠ΄ΠΈΠ»ΠΈ Ρ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ΠΌ ΠΎΠ±ΠΎΡΡΠ΄ΠΎΠ²Π°Π½ΠΈΡ Π¦Π΅Π½ΡΡΠΎΠ² ΠΊΠΎΠ»Π»Π΅ΠΊΡΠΈΠ²Π½ΠΎΠ³ΠΎ ΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΡ Β«ΠΠ·ΠΎΡΠΎΠΏΠ½ΠΎ-Π³Π΅ΠΎΡ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠΉΒ» ΠΠΠ₯ Π‘Π Π ΠΠ ΠΈ Β«ΠΠ΅ΠΎΠ΄ΠΈΠ½Π°ΠΌΠΈΠΊΠ° ΠΈ Π³Π΅ΠΎΡ
ΡΠΎΠ½ΠΎΠ»ΠΎΠ³ΠΈΡΒ» ΠΠΠ Π‘Π Π ΠΠ. ΠΠ²ΡΠΎΡΡ Π²ΡΡΠ°ΠΆΠ°ΡΡ Π±Π»Π°Π³ΠΎΠ΄Π°ΡΠ½ΠΎΡΡΡ Π²Π΅Π΄ΡΡΠ΅ΠΌΡ ΠΈΠ½ΠΆΠ΅Π½Π΅ΡΡ ΠΠΠ Π‘Π Π ΠΠ Π‘.Π. ΠΠ°Π½ΡΠ΅Π΅Π²ΠΎΠΉ Π·Π° ΠΏΡΠΎΠ²Π΅Π΄Π΅Π½ΠΈΠ΅ ICP-MS Π°Π½Π°Π»ΠΈΠ·Π° ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ ΠΈ Π²Π΅Π΄ΡΡΠ΅ΠΌΡ ΠΈΠ½ΠΆΠ΅Π½Π΅ΡΡ ΠΠΠ₯ Π‘Π Π ΠΠ Π.Π. ΠΠΎΠ³ΡΠ΄ΠΈΠ½ΠΎΠΉ Π·Π° ΠΎΠΏΡΠ΅Π΄Π΅Π»Π΅Π½ΠΈΠ΅ ΠΏΠΎΡΠΎΠ΄ΠΎΠΎΠ±ΡΠ°Π·ΡΡΡΠΈΡ
ΠΎΠΊΡΠΈΠ΄ΠΎΠ² Π² ΠΎΠ±ΡΠ°Π·ΡΠ°Ρ
ΠΊΠ΅ΡΠ°ΠΌΠΈΠΊΠΈ.Current work was carried out with the financial support of the Russian Science Foundation (grant No. 19-78-10084). All measurements were performed using the equipment of βIsotope-Geochemical Researchβ and βGeodynamics and Geochronologyβ Joint Use Centers of the Siberian Branch of the Russian Academy of Sciences. The authors are grateful to Svetlana Panteeva for ICPMS analysis and Galina Pogudina for the determination of rock-forming oxides in ceramic samples
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