235 research outputs found
ΠΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΠ΅ Π·Π°ΠΊΠΎΠ½ΠΎΠΌΠ΅ΡΠ½ΠΎΡΡΠ΅ΠΉ ΡΠ°Π·Π²ΠΈΡΠΈΡ ΡΡΡΡΠΊΡΡΡΠ½ΠΎ-Ρ ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΎΠΉ Π½Π΅ΠΎΠ΄Π½ΠΎΡΠΎΠ΄Π½ΠΎΡΡΠΈ Π² ΡΠ°Π·Π½ΠΎΡΠΎΠ΄Π½ΠΎΠΌ ΡΠ²Π°ΡΠ½ΠΎΠΌ ΡΠΎΠ΅Π΄ΠΈΠ½Π΅Π½ΠΈΠΈ ΡΡΡΠ±ΠΎΠΏΡΠΎΠ²ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΠΏΠ΅ΡΠ΅Ρ ΠΎΠ΄Π½ΠΈΠΊΠ°
ΠΠ°Π½Π½Π°Ρ ΡΠ°Π±ΠΎΡΠ° ΠΏΠΎΡΠ²ΡΡΠ΅Π½Π° ΠΈΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΡΡΡΡΠΊΡΡΡΠ½ΠΎ-Ρ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΎΠΉ Π½Π΅ΠΎΠ΄Π½ΠΎΡΠΎΠ΄Π½ΠΎΡΡΠΈ (Π‘Π₯Π) ΡΡΡΠ±ΠΎΠΏΡΠΎΠ²ΠΎΠ΄Π½ΠΎΠ³ΠΎ ΠΏΠ΅ΡΠ΅Ρ
ΠΎΠ΄Π½ΠΈΠΊΠ° ΠΈΠ· ΡΠ°Π·Π½ΠΎΡΠΎΠ΄Π½ΡΡ
ΡΡΠ°Π»Π΅ΠΉ, Π²ΡΠΏΠΎΠ»Π½Π΅Π½Π½ΠΎΠ³ΠΎ Π°ΡΠ³ΠΎΠ½ΠΎΠ΄ΡΠ³ΠΎΠ²ΠΎΠΉ ΡΠ²Π°ΡΠΊΠΎΠΉ (ΠΡΠΠ‘). ΠΡΠΈ ΠΏΠΎΠΌΠΎΡΠΈ ΠΎΠΏΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΌΠΈΠΊΡΠΎΡΠΊΠΎΠΏΠ° ΠΏΠΎΠ»ΡΡΠ΅Π½Ρ ΡΠΎΡΠΎΠ³ΡΠ°ΡΠΈΠΈ Π‘Π₯Π ΠΈ Π΅Π΅ ΡΠ°Π·ΠΌΠ΅ΡΡ. Π‘Π₯Π Π²ΡΡΠ°ΠΆΠ°Π΅ΡΡΡ Π² ΠΏΠΎΡΠ²Π»Π΅Π½ΠΈΠΈ ΠΏΡΠΎΡΠ»ΠΎΠ΅ΠΊ (ΠΊΠ°ΡΠ±ΠΈΠ΄Π½ΠΎΠΉ ΠΈ ΡΠ΅ΡΡΠΈΡΠ½ΠΎΠΉ) Ρ ΡΠ°Π·Π½ΡΠΌ Ρ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΈΠΌ ΡΠΎΡΡΠ°Π²ΠΎΠΌ. ΠΡΠΈΠ²Π΅Π΄Π΅Π½Ρ Π³ΡΠ°ΡΠΈΠΊΠΈ ΡΠΎΡΡΠ° ΡΠΈΡΠΈΠ½ ΠΏΡΠΎΡΠ»ΠΎΠ΅ΠΊ ΠΎΡ Π²ΡΠ΅ΠΌΠ΅Π½ΠΈ Π²ΡΠ΄Π΅ΡΠΆΠΊΠΈ ΠΈ ΡΠ΅ΠΌΠΏΠ΅ΡΠ°ΡΡΡΡ.This paper is devoted to the comparison of the structural and chemical inhomogeneity (SCI) of adapters made of dissimilar steels, made by tungsten insert gas (TIG). By means of optical microscope, photographs of the SCI and its dimensions were obtained. SCI is expressed in the appearance of interlayers (carbide and ferritic) with different chemical composition. Graphs of the growth of the widths of the interlayers from the time of exposure and temperature are given
ΠΠΎΡΠΈΡΡΠ°Ρ ΡΡΡΡΠΊΡΡΡΠ° ΠΏΡΠΎΠ΄ΡΠΊΡΠΎΠ² ΡΠ»Π΅ΠΊΡΡΠΎΡ ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠΈΠ½ΡΠ΅Π·Π° Π½Π° ΠΏΠ΅ΡΠ΅ΠΌΠ΅Π½Π½ΠΎΠΌ ΡΠΎΠΊΠ΅ Π½Π°Π½ΠΎΠ΄ΠΈΡΠΏΠ΅ΡΡΠ½ΡΡ ΠΎΠΊΡΠΈΠ΄ΠΎΠ² ΠΎΠ»ΠΎΠ²Π°
ΠΠ΅ΡΠΎΠ΄Π°ΠΌΠΈ ΡΠ»Π΅ΠΊΡΡΠΎΠ½Π½ΠΎΠΉ ΠΌΠΈΠΊΡΠΎΡΠΊΠΎΠΏΠΈΠΈ ΠΈ Π½ΠΈΠ·ΠΊΠΎΡΠ΅ΠΌΠΏΠ΅ΡΠ°ΡΡΡΠ½ΠΎΠΉ Π°Π΄ΡΠΎΡΠ±ΡΠΈΠΈ Π°Π·ΠΎΡΠ° ΠΈΠ·ΡΡΠ΅Π½Π° ΠΏΠΎΡΠΈΡΡΠ°Ρ ΡΡΡΡΠΊΡΡΡΠ° ΠΏΡΠΎΠ΄ΡΠΊΡΠΎΠ² ΡΠ»Π΅ΠΊΡΡΠΎΠ»ΠΈΠ·Π° ΠΌΠ΅ΡΠ°Π»Π»ΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΎΠ»ΠΎΠ²Π° Π½Π° ΠΏΠ΅ΡΠ΅ΠΌΠ΅Π½Π½ΠΎΠΌ ΡΠΎΠΊΠ΅ ΠΏΡΠΎΠΌΡΡΠ»Π΅Π½Π½ΠΎΠΉ ΡΠ°ΡΡΠΎΡΡ. Π£ΡΡΠ°Π½ΠΎΠ²Π»Π΅Π½ΠΎ, ΡΡΠΎ ΠΏΡΠΎΠ΄ΡΠΊΡΡ ΡΠΈΠ½ΡΠ΅Π·Π° Ρ
Π°ΡΠ°ΠΊΡΠ΅ΡΠΈΠ·ΡΡΡΡΡ Π²ΡΡΠΎΠΊΠΈΠΌΠΈ Π·Π½Π°ΡΠ΅Π½ΠΈΡΠΌΠΈ ΡΠ΄Π΅Π»ΡΠ½ΠΎΠΉ ΠΏΠ»ΠΎΡΠ°Π΄ΠΈ ΠΏΠΎΠ²Π΅ΡΡ
Π½ΠΎΡΡΠΈ ΠΈ ΠΌΠ΅Π·Π°ΠΏΠΎΡΠΈΡΡΠΎΠΉ ΡΡΡΡΠΊΡΡΡΠΎΠΉ. ΠΠΎΠΊΠ°Π·Π°Π½ΠΎ, ΡΡΠΎ ΡΡΠ΅Π΄Π½ΠΈΠΉ ΡΠ°Π·ΠΌΠ΅Ρ ΡΠ°ΡΡΠΈΡ Π²Π°ΡΡΠΈΡΡΠ΅Ρ Π² ΠΈΠ½ΡΠ΅ΡΠ²Π°Π»Π΅ 10β¦30 Π½ΠΌ
Advanced Diagnostics for the Study of Linearly Polarized Emission. II: Application to Diffuse Interstellar Radio Synchrotron Emission
Diagnostics of polarized emission provide us with valuable information on the
Galactic magnetic field and the state of turbulence in the interstellar medium,
which cannot be obtained from synchrotron intensity alone. In Paper I (Herron
et al. 2017b), we derived polarization diagnostics that are rotationally and
translationally invariant in the - plane, similar to the polarization
gradient. In this paper, we apply these diagnostics to simulations of ideal
magnetohydrodynamic turbulence that have a range of sonic and Alfv\'enic Mach
numbers. We generate synthetic images of Stokes and for these
simulations, for the cases where the turbulence is illuminated from behind by
uniform polarized emission, and where the polarized emission originates from
within the turbulent volume. From these simulated images we calculate the
polarization diagnostics derived in Paper I, for different lines of sight
relative to the mean magnetic field, and for a range of frequencies. For all of
our simulations, we find that the polarization gradient is very similar to the
generalized polarization gradient, and that both trace spatial variations in
the magnetoionic medium for the case where emission originates within the
turbulent volume, provided that the medium is not supersonic. We propose a
method for distinguishing the cases of emission coming from behind or within a
turbulent, Faraday rotating medium, and a method to partly map the rotation
measure of the observed region. We also speculate on statistics of these
diagnostics that may allow us to constrain the physical properties of an
observed turbulent region.Comment: 34 pages, 25 figures, accepted for publication in Ap
An XMM-Newton view of the extended "filament" near the cluster of galaxies Abell 85
We have observed with XMM-Newton the extended 4 Mpc filament detected by the
ROSAT PSPC in the neighbourhood of the cluster of galaxies Abell 85. We confirm
that there is an extended feature, aligned at the same position angle as the
major axis of the central cD, the bright cluster galaxies, and nearby groups
and clusters. We find that the X-ray emission from the filament is best
described by thermal emission with a temperature of about 2 keV, which is
significantly lower than the ambient cluster medium, but is significantly
higher than anticipated for a gas in a weakly bound extended filament. It is
not clear whether this is a filament of diffuse emission, a chain of several
groups of galaxies, or stripped gas from the infalling south blob.Comment: accepted for publication in Astronomy & Astrophysics Letter
The richest superclusters. I. Morphology
We study the morphology of the richest superclusters from the catalogues of
superclusters of galaxies in the 2dF Galaxy Redshift Survey and compare the
morphology of real superclusters with model superclusters in the Millennium
Simulation. We use Minkowski functionals and shapefinders to quantify the
morphology of superclusters: their sizes, shapes, and clumpiness. We generate
empirical models of simple geometry to understand which morphologies correspond
to the supercluster shapefinders. We show that rich superclusters have
elongated, filamentary shapes with high-density clumps in their core regions.
The clumpiness of superclusters is determined using the fourth Minkowski
functional . In the - shapefinder plane the morphology of
superclusters is described by a curve which is characteristic to
multi-branching filaments. We also find that the differences between the fourth
Minkowski functional for the bright and faint galaxies in observed
superclusters are larger than in simulated superclusters.Comment: 14 pages, 8 figures, submitted to Astronomy and Astrophysic
Search for non-Gaussianity in pixel, harmonic and wavelet space: compared and combined
We present a comparison between three approaches to test non-Gaussianity of
cosmic microwave background data. The Minkowski functionals, the empirical
process method and the skewness of wavelet coefficients are applied to maps
generated from non-standard inflationary models and to Gaussian maps with point
sources included. We discuss the different power of the pixel, harmonic and
wavelet space methods on these simulated almost full-sky data (with Planck like
noise). We also suggest a new procedure consisting of a combination of
statistics in pixel, harmonic and wavelet space.Comment: Accepted for publication in PR
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