429 research outputs found
Comprehensive study of physical and chemical behavior of vanadium in molten alkali metal chlorides
ΠΠ»Π΅ΠΊΡΡΠΎΠ΄Π½ΡΠ΅ ΠΏΡΠΎΡΠ΅ΡΡΡ Ρ ΡΡΠ°ΡΡΠΈΠ΅ΠΌ ΡΠΎΠ΅Π΄ΠΈΠ½Π΅Π½ΠΈΠΉ Π²Π°Π½Π°Π΄ΠΈΡ Π±ΡΠ»ΠΈ ΠΈΠ·ΡΡΠ΅Π½Ρ ΠΏΡΠΈ 690-860 oC Π² ΡΠ°ΡΠΏΠ»Π°Π²Π°Ρ
Π½Π° ΠΎΡΠ½ΠΎΠ²Π΅ (Na-K)ClΡΠΊΠ² Ρ ΠΈΡΠΏΠΎΠ»ΡΠ·ΠΎΠ²Π°Π½ΠΈΠ΅ΠΌ ΡΠ»Π΅ΠΊΡΡΠΎΡ
ΠΈΠΌΠΈΡΠ΅ΡΠΊΠΈΡ
ΡΡΠ°ΡΠΈΠΎΠ½Π°ΡΠ½ΡΡ
ΠΈ Π½Π΅ΡΡΠ°ΡΠΈΠΎΠ½Π°ΡΠ½ΡΡ
ΠΌΠ΅ΡΠΎΠ΄ΠΎΠ²: Ρ
ΡΠΎΠ½ΠΎΠ°ΠΌΠΏΠ΅ΡΠΎΠΌΠ΅ΡΡΠΈΡ, Ρ
ΡΠΎΠ½ΠΎΠΏΠΎΡΠ΅Π½ΡΠΈΠΎΠΌΠ΅ΡΡΠΈΡ, ΡΠΈΠΊΠ»ΠΈΡΠ΅ΡΠΊΠ°Ρ ΠΈ ΠΊΠ²Π°Π΄ΡΠ°ΡΠ½ΠΎ-Π²ΠΎΠ»Π½ΠΎΠ²Π°Ρ Π²ΠΎΠ»ΡΡΠ°ΠΌΠΏΠ΅ΡΠΎΠΌΠ΅ΡΡΠΈΡ. ΠΠ°ΡΠΎΠ΄Π½ΠΎΠ΅ Π²ΠΎΡΡΡΠ°Π½ΠΎΠ²Π»Π΅Π½ΠΈΠ΅ Π²Π°Π½Π°Π΄ΠΈΡ Π² ΡΠ°ΡΠΏΠ»Π°Π²Π°Ρ
(Na-K)ClΡΠΊΠ²-VCl3 Π²ΠΊΠ»ΡΡΠ°Π΅Ρ 2 ΡΡΠ°Π΄ΠΈΠΈ: ΠΎΠ΄Π½ΠΎΡΠ»Π΅ΠΊΡΡΠΎΠ½Π½Π°Ρ V3+βV2+ ΠΈ Π΄Π²ΡΡ
ΡΠ»Π΅ΠΊΡΡΠΎΠ½Π½Π°Ρ V2+βV ΡΠ΅Π°ΠΊΡΠΈΠΈ. ΠΡΠΈ ΠΏΠΎΡΡΠΎΡΠ½Π½ΠΎ ΠΏΡΠΈΠ»ΠΎΠΆΠ΅Π½Π½ΠΎΠΌ ΡΠΎΠΊΠ΅ ΠΎΠ±Π΅ ΡΡΠ°Π΄ΠΈΠΈ ΠΊΠΎΠ½ΡΡΠΎΠ»ΠΈΡΡΡΡΡΡ Π΄ΠΈΡΡΡΠ·ΠΈΠ΅ΠΉ. ΠΠ΅Ρ
Π°Π½ΠΈΠ·ΠΌ ΡΠ»Π΅ΠΊΡΡΠΎΠ΄Π½ΡΡ
ΡΠ΅Π°ΠΊΡΠΈΠΉ ΠΎΡΡΠ°Π΅ΡΡΡ ΡΡ
ΠΎΠ΄Π½ΡΠΌ ΠΏΡΠΈ Π²ΠΎΠ»ΡΡΠ°ΠΌΠΏΠ΅ΡΠΎΠΌΠ΅ΡΡΠΈΡΠ΅ΡΠΊΠΈΡ
ΠΈΠ·ΠΌΠ΅ΡΠ΅Π½ΠΈΡΡ
Π½Π° ΡΠΊΠΎΡΠΎΡΡΡΡ
ΡΠ°Π·Π²Π΅ΡΡΠΊΠΈ Π½ΠΈΠΆΠ΅ 200 ΠΌΠ/Ρ. ΠΡΠΈ Π²ΡΡΠΎΠΊΠΈΡ
ΡΠΊΠΎΡΠΎΡΡΡΡ
ΡΠ°Π·Π²Π΅ΡΡΠΊΠΈ ΠΏΠΎΡΠ΅Π½ΡΠΈΠ°Π»Π° ΡΠ΅Π°ΠΊΡΠΈΠΈ ΠΏΡΠΎΡΠ΅ΠΊΠ°ΡΡ Π² ΡΠΌΠ΅ΡΠ°Π½Π½ΠΎΠΌ Π΄ΠΈΡΡΡΠ·ΠΈΠΎΠ½Π½ΠΎ-ΠΊΠΈΠ½Π΅ΡΠΈΡΠ΅ΡΠΊΠΎΠΌ ΡΠ΅ΠΆΠΈΠΌΠ΅. ΠΠ½Π°Π»ΠΈΠ· ΠΠ-ΠΏΡΠΎΡΠ΅ΡΡΠΎΠ² Π² Ρ
Π»ΠΎΡΠΈΠ΄Π½ΡΡ
ΡΠ°ΡΠΏΠ»Π°Π²Π°Ρ
ΠΏΠΎΠΊΠ°Π·Π°Π», ΡΡΠΎ ΠΊΠΎΠΌΠΏΠ»Π΅ΠΊΡΠ½ΡΠ΅ ΠΈΠΎΠ½Ρ V(II) ΠΈ V(III) ΡΡΡΠΎΠΉΡΠΈΠ²Ρ Π² Π΄Π°Π½Π½ΡΡ
ΡΡΠ΅Π΄Π°Ρ
.The electrode processes involving vanadium species were studied at 690-860 oC in NaCl-KCl-based melts employing electrochemical stationary and non-stationary methods: chronoamperometry, chronopotentiometry, cyclic and square-wave voltammetry. Cathodic reduction of vanadium in VCl3-NaCl-KCl melts involves two steps: one-electron V3+βV2+ and two-electron V2+βV reactions. Under a constant applied current both stages are diffusion-controlled. The mechanism of the electrode reactions remains the same in voltammetry measurements at polarization rates below ca. 200 mV/sec. At higher potential scan rates the reactions proceed in a mixed diffusion- and kinetic-controlled regime. Analysis of the red-ox processes in chloride melts showed that V(II) and V(III) complex chloride ions are stable in these media.ΠΡΠΎΠ³ΡΠ°ΠΌΠΌΠ° ΡΠ°Π·Π²ΠΈΡΠΈΡ Π£ΡΠ€Π£ Π½Π° 2013 Π³ΠΎΠ΄ (ΠΏ.2.1.1.1
LEADING ATOPIC PATHOLOGIES IN CHILDREN ON THE TERRITORY OF MYKOLAIV REGION
The article is devoted to allergic diseases among children of the Nikolaev area, first of all bronchial asthma of an atopic form.Β The dynamics of the prevalence of allergic diseases is analyzed, the most rational methods of diagnosis and treatment of allergopathology are determined.Β Data on hospitalization in the allergy department, the structure of diagnoses that are most often clinically established in children with allergy pathology are presented.Β The materials will be of interest to allergists, pulmonologists, immunologists, family doctors and pediatricians.Key words: allergy, bronchial asthma, allergic diseases, atopy, allergology, pediatrics
Multi-wavelength Emission from the Fermi Bubble III. Stochastic (Fermi) Re-Acceleration of Relativistic Electrons Emitted by SNRs
We analyse the model of stochastic re-acceleration of electrons, which are
emitted by supernova remnants (SNRs) in the Galactic Disk and propagate then
into the Galactic halo, in order to explain the origin on nonthermal (radio and
gamma-ray) emission from the Fermi Bubbles (FB). We assume that the energy for
re-acceleration in the halo is supplied by shocks generated by processes of
star accretion onto the central black hole. Numerical simulations show that
regions with strong turbulence (places for electron re-acceleration) are
located high up in the Galactic Halo about several kpc above the disk. The
energy of SNR electrons that reach these regions does not exceed several GeV
because of synchrotron and inverse Compton energy losses. At appropriate
parameters of re-acceleration these electrons can be re-accelerated up to the
energy 10E12 eV which explains in this model the origin of the observed radio
and gamma-ray emission from the FB. However although the model gamma-ray
spectrum is consistent with the Fermi results, the model radio spectrum is
steeper than the observed by WMAP and Planck. If adiabatic losses due to plasma
outflow from the Galactic central regions are taken into account, then the
re-acceleration model nicely reproduces the Planck datapoints.Comment: 33 pages, 8 figures, accepted by Ap
Analytical and numerical studies of central galactic outflows powered by tidal disruption events -- a model for the Fermi bubbles?
Capture and tidal disruption of stars by the supermassive black hole in the
Galactic center (GC) should occur regularly. The energy released and dissipated
by this processes will affect both the ambient environment of the GC and the
Galactic halo. A single star of super-Eddington eruption generates a subsonic
out ow with an energy release of more than erg, which still is not
high enough to push shock heated gas into the halo. Only routine tidal
disruption of stars near the GC can provide enough cumulative energy to form
and maintain large scale structures like the Fermi Bubbles. The average rate of
disruption events is expected to be ~ yr, providing
the average power of energy release from the GC into the halo of dW/dt ~
3*10 erg/s, which is needed to support the Fermi Bubbles. The GC black
hole is surrounded by molecular clouds in the disk, but their overall mass and
filling factor is too low to stall the shocks from tidal disruption events
significantly. The de facto continuous energy injection on timescales of Myr
will lead to the propagation of strong shocks in a density stratified Galactic
halo and thus create elongated bubble-like features, which are symmetric to the
Galactic midplane.Comment: 11 pages, 5 figures. The title and abstract have been changed.
Accepted by Astrophysical Journa
Particle acceleration and the origin of gamma-ray emission from Fermi Bubbles
Fermi LAT has discovered two extended gamma-ray bubbles above and below the
galactic plane. We propose that their origin is due to the energy release in
the Galactic center (GC) as a result of quasi-periodic star accretion onto the
central black hole. Shocks generated by these processes propagate into the
Galactic halo and accelerate particles there. We show that electrons
accelerated up to ~10 TeV may be responsible for the observed gamma-ray
emission of the bubbles as a result of inverse Compton (IC) scattering on the
relic photons. We also suggest that the Bubble could generate the flux of CR
protons at energies > 10^15 eV because the shocks in the Bubble have much
larger length scales and longer lifetimes in comparison with those in SNRs.
This may explain the the CR spectrum above the knee.Comment: 5 pages, 4 figures. Expanded version of the contribution to the 32nd
ICRC, Beijing, #0589. To appear in the proceeding
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