729 research outputs found
Q-phonon description of low lying 1^- two-phonon states in spherical nuclei
The properties of 1^-_1 two-phonon states and the characteristics of E1
transition probabilities between low-lying collective states in spherical
nuclei are analysed within the Q-phonon approach to the description of
collective states. Several relations between observables are obtained.
Microscopic calculations of the E1 0^+_1 -> 1^-_1 transition matrix elements
are performed on the basis of the RPA. A satisfactory description of the
experimental data is obtained.Comment: 16 pages, 2 figures, 9 table
Vela X-1 as a laboratory for accretion in High-Mass X-ray Binaries
Vela X-1 is an eclipsing high mass X-ray binary (HMXB) consisting of a 283s
accreting X-ray pulsar in a close orbit of 8.964 days around the B0.5Ib
supergiant HD77581 at a distance of just 2.4 kpc. The system is considered a
prototype of wind-accreting HMXB and it has been used as a baseline in
different theoretical or modelling studies.
We discuss the observational properties of the system and the use of the
observational data as laboratory to test recent developments in modelling the
accretion process in High-Mass X-ray Binaries (e.g., Sander et al. 2018; El
Mellah et al. 2018), which range from detailed descriptions of the wind
acceleration to modelling of the structure of the flow of matter close to the
neutron star and its variations.Comment: 4 pages, 2 figures, proceedings of the 12th INTEGRAL conference
"INTEGRAL looks AHEAD to Multimessenger astronomy" in Geneva (Switzerland) on
11-15 February 201
Long term variability of Cygnus X-1: VII. Orbital variability of the focussed wind in Cyg X-1 / HDE 226868 system
Binary systems with an accreting compact object are a unique chance to
investigate the strong, clumpy, line-driven winds of early type supergiants by
using the compact object's X-rays to probe the wind structure. We analyze the
two-component wind of HDE 226868, the O9.7Iab giant companion of the black hole
Cyg X-1 using 4.77 Ms of RXTE observations of the system taken over the course
of 16 years. Absorption changes strongly over the 5.6 d binary orbit, but also
shows a large scatter at a given orbital phase, especially at superior
conjunction. The orbital variability is most prominent when the black hole is
in the hard X-ray state. Our data are poorer for the intermediate and soft
state, but show signs for orbital variability of the absorption column in the
intermediate state. We quantitatively compare the data in the hard state to a
toy model of a focussed Castor-Abbott-Klein-wind: as it does not incorporate
clumping, the model does not describe the observations well. A qualitative
comparison to a simplified simulation of clumpy winds with spherical clumps
shows good agreement in the distribution of the equivalent hydrogen column
density for models with a porosity length on the order of the stellar radius at
inferior conjunction; we conjecture that the deviations between data and model
at superior conjunction could be either due to lack of a focussed wind
component in the model or a more complicated clump structure.Comment: proposed for acceptance in A&A, 11 pages, 11 figures (two in
appendix
Morphological Criteria for Diagnosis of Pulmonary Lesions of Lungs in Tumors Based on Resection Material
Morphological criteria of diagnosis of dust lesions of lungs in tumors on resectionmaterial are considered in the article. It is shown that the complex application of various research methods allows the identification of dust particles in the lung and lymph node tissues, and contributes to the improvement of the diagnosis of dust lesions of the respiratory system. Morphological characteristics of bauxite pneumoconiosis in primary lung cancer on resection material are presented
Diffusion spin echo decay by pulsed magnetic field gradient NMR and some structure features in blockcopolymer solutions
Blockcopolymer solutions were investigated by pulsed field gradient NMR. Nonexponential diffusion decay of solvent molecules and the dependence of it's shape on time of observation uere found out. These features (unusual for solvent molecules) were explained on assumption of the solution heterogeneous structure. Consideration, performed, allow us to estimate the linear dimensions of the heterogeneities, which for concentrated systems occured to be near 10000 A. © 1985 Springer-Verlag
Population of isomers in decay of the giant dipole resonance
The value of an isomeric ratio (IR) in N=81 isotones (Ba, Ce,
Nd and Sm) is studied by means of the ( reaction.
This quantity measures a probability to populate the isomeric state in respect
to the ground state population. In ( reactions, the giant dipole
resonance (GDR) is excited and after its decay by a neutron emission, the
nucleus has an excitation energy of a few MeV. The forthcoming decay
by direct or cascade transitions deexcites the nucleus into an isomeric or
ground state. It has been observed experimentally that the IR for Ba
and Ce equals about 0.13 while in two heavier isotones it is even less
than half the size. To explain this effect, the structure of the excited states
in the energy region up to 6.5 MeV has been calculated within the Quasiparticle
Phonon Model. Many states are found connected to the ground and isomeric states
by , and transitions. The single-particle component of the wave
function is responsible for the large values of the transitions. The calculated
value of the isomeric ratio is in very good agreement with the experimental
data for all isotones. A slightly different value of maximum energy with which
the nuclei rest after neutron decay of the GDR is responsible for the reported
effect of the A-dependence of the IR.Comment: 16 pages, 4 Fig
LABORATORY MEASUREMENTS OF THE K-SHELL TRANSITION ENERGIES IN L-SHELL IONS OF SI AND S
We have measured the energies of the strongest 1s–2ℓ (ℓ = s, p) transitions in He- through Ne-like silicon and sulfur ions to an accuracy of <1 eV using the Lawrence Livermore National Laboratory's electron beam ion traps, EBIT-I and SuperEBIT, and the NASA/GSFC EBIT Calorimeter Spectrometer (ECS). We identify and measure the energies of 18 and 21 X-ray features from silicon and sulfur, respectively. The results are compared to new Flexible Atomic Code calculations and to semi-relativistic Hartree–Fock calculations by Palmeri et al. (2008). These results will be especially useful for wind diagnostics in high-mass X-ray binaries, such as Vela X-1 and Cygnus X-1, where high-resolution spectral measurements using Chandra's high-energy transmission grating has made it possible to measure Doppler shifts of 100 km s[superscript -1]. The accuracy of our measurements is consistent with that needed to analyze Chandra observations, exceeding Chandra's 100 km s[superscript -1] limit. Hence, the results presented here not only provide benchmarks for theory, but also accurate rest energies that can be used to determine the bulk motion of material in astrophysical sources. We show the usefulness of our results by applying them to redetermine Doppler shifts from Chandra observations of Vela X-1.United States. National Aeronautics and Space Administration (work orders NNX/2AH84G)United States. Department of Energy (Contract DE-AC52-07NA27344)Smithsonian Astrophysical Observatory (contract SV3-73016
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