No abstract available

[en] Localisation of the accessory mammary gland with mammography examination is discussed

[en] The NPI CFNF was developed for the fast neutron research employing the AVF cyclotron U-120M (K=40). We have taken the unique advantage of two possible ion-acceleration regimes of the NPI cyclotron operation, i.e. the beams of H⁺(24MeV), D⁺(17 MeV) and ³He⁺⁺ (40 MeV) ions with well defined spectral characteristics and also the high-current beams from the acceleration of H^-(37 MeV) and D^-(18 MeV) ions. Utilizing the pulse-height unfolding technique, the deuteron break-up processes initiated by 37 MeV protons and/or 40 MeV ³He-ions were experimentally verified as the most suitable source reactions for producing a white-spectrum neutron field with the mean energy of about 14 MeV and the energy range up to 34 MeV. These observables well simulate a dominant part of neutron spectrum from the d+Li source reaction of the IFMIF (International Fusion Material Irradiation Facility). Employing the heavy-water target, the neutron sources of the IFMIF-like spectrum are routinely operated. Present report illustrates the capability of the NPI CFNF to provide a suitable tool for a wide class of experiments relevant to the IFMIF neutronic calculations. (author)

[en] The results of analysis of nuclear reaction properties, which can be used for fast neutron production at the U-120M isochronous cyclotron, are presented. The aim of the analysis carried out is to find optimal conditions for the generation of intense neutron beams with the energy upto 20 MeV, as well as to obtain data on energy distribution and the mean neutron energy in a beam

[en] The NPI FNF was developed for the fast neutron research employing the AVF cyclotron U-120M (K = 40). We have taken the unique advantage of two possible ion-acceleration regimes of the NPI cyclotron operation, i.e. the beams of H⁺(24 MeV), D⁺(17 MeV) and ³ He⁺⁺ (40 MeV) ions with well defined spectral characteristics and also the high-current beams from the acceleration of H^- (37 MeV) and D^- (18 MeV) ions. Utilizing the pulse-height unfolding technique, the deuteron break-up processes were experimentally verified as the most suitable source reactions for producing the white-spectrum neutrons with the mean energy of about 14 MeV and the energy range up to 34 MeV. These observables well simulate a dominant part of neutron spectrum from the d + Li source reaction of the IFMIF (International Fusion Material Irradiation Facility). Employing the proton beam (37 MeV) and the heavy-water-flow target, the neutron source of the IFMIF-like spectrum with the source power up to 6 x 10¹¹ n/sr/s is routinely operated. The resent report describes in details the capability of the NPI FNF to provide a suitable tool for a wide class of the neutron spectrometry-, the neutron transport- and the activation benchmark experiments relevant to the IFMIF neutronic calculations. (authors)

No abstract available

[en] The ²⁰Ne(p,γ)²¹Na reaction rate at stellar energies is dominated by capture to the ground state through the tail of a subthreshold resonance state at an excitation energy of 2425 keV in ²¹Na. Both resonant and direct capture contribute to the reaction rate while direct captures to other bound states are negligible. The overall normalization of direct capture to the subthreshold state is determined by the asymptotic normalization coefficient (ANC). Simultaneously this ANC determines the proton partial width of the subthreshold resonance state. To determine the ANC, the ²⁰Ne(³He,d)²¹Na proton transfer reaction has been measured, at an incident energy of 25.83 MeV. Angular distributions for proton transfer to the ground and first three excited states were measured, and ANCs were then extracted from comparison with distorted-wave Born approximation calculations. Using these ANCs, we calculated the astrophysical factor for ²⁰Ne(p,γ)²¹Na. Our total astrophysical factor is S(0)=5900±1200 keV b. Our analysis confirms that only nonresonant and resonant captures through the subthreshold state are important

No abstract available

[en] The ¹⁵N(p,γ)¹⁶O reaction provides a path from the CN cycle to the CNO bi-cycle and CNO tri-cycle. The measured astrophysical factor for this reaction is dominated by resonant capture through two strong J^π=1^- resonances at E_R=312 and 962 keV and direct capture to the ground state. Asymptotic normalization coefficients (ANCs) for the ground and seven excited states in ¹⁶O were extracted from the comparison of experimental differential cross sections for the ¹⁵N(³He,d)¹⁶O reaction with distorted-wave Born approximation calculations. Using these ANCs and proton and α resonance widths determined from an R-matrix fit to the data from the ¹⁵N(p,α)¹²C reaction, we carried out an R-matrix calculation to obtain the astrophysical factor for the ¹⁵N(p,γ)¹⁶O reaction. The results indicate that the direct capture contribution was previously overestimated. We find the astrophysical factor to be S(0)=36.0±6.0 keV b, which is about a factor of 2 lower than the presently accepted value. We conclude that for every 2200±300 cycles of the main CN cycle one CN catalyst is lost due to this reaction