24 research outputs found
Change of nuclear configurations in the neutrinoless double- decay of Te Xe and Xe Ba
The change in the configuration of valence protons between the initial and
final states in the neutrinoless double- decay of Te
Xe and of Xe Ba has been
determined by measuring the cross sections of the (,He) reaction with
101-MeV deuterons. Together with our recent determination of the relevant
neutron configurations involved in the process, a quantitative comparison with
the latest shell-model and interacting-boson-model calculations reveals
significant discrepancies. These are the same calculations used to determine
the nuclear matrix elements governing the rate of neutrinoless double-
decay in these systems.Comment: 10 pages, 4 figures, 9 table
Neutron occupancies and single-particle energies across the stable tin isotopes
The occupancies and vacancies of the valence neutron orbitals across the
stable tin isotopic chain from have been determined. These
were inferred from the cross sections of neutron-adding and -removing
reactions. In each case, the reactions were chosen to have good
angular-momentum matching for transfer to the low- and high- orbitals
present in this valence space. These new data are compared to older systematic
studies. The effective single-neutron energies are determined by combining
information from energy centroids determined from the adding and removing
reactions. Two of the five orbitals are nearly degenerate, below , and
approximately two MeV more bound than the other three, which are also
degenerate.Comment: 11 pages, 10 figure
UltraCarbonaceous Antarctic micrometeorites, probing the Solar System beyond the nitrogen snow-line
We investigate UltraCarbonaceous Antarctic micrometeorites composition. * They reveal a new N-rich organic matter from the Solar System. * This exceptional organic matter is formed in the Oort cloud. * Cosmic ray irradiation form this carbon nitride organic material. * A nitrogen rich snow line must exists in our Solar System
Interstellar and interplanetary solids in the laboratory
International audienceThe composition of the interstellar matter is driven by environmental parameters (e.g. elemental abundance, density, reactant nature, radiations, temperature, time scales) and results also from external interstellar medium physico-chemical conditions. Astrochemists must rely on remote observations to monitor and analyze the comÂposition of interstellar solids. These observations give essentially access to the molecular functionality of the solids, rarely elemental composition constraints and isotopic fractionation only in the gas phase. Astrochemists bring additional information from the study of analogues produced in the laboratory, placed in simulated space environments. Planetologists and cosmochemists can have access and spectroscopically examine collected extra-terrestrial material directly in the laboratory. Observations of the diffuse interstellar medium (DISM) and molecular clouds (MC) set constraints on the composition of organic solids and large molecules, that! can then be compared with collected extraterrestrial materials analyses, to shed light on their possible links
Interstellar and interplanetary solids in the laboratory
International audienceThe composition of the interstellar matter is driven by environmental parameters (e.g. elemental abundance, density, reactant nature, radiations, temperature, time scales) and results also from external interstellar medium physico-chemical conditions. Astrochemists must rely on remote observations to monitor and analyze the comÂposition of interstellar solids. These observations give essentially access to the molecular functionality of the solids, rarely elemental composition constraints and isotopic fractionation only in the gas phase. Astrochemists bring additional information from the study of analogues produced in the laboratory, placed in simulated space environments. Planetologists and cosmochemists can have access and spectroscopically examine collected extra-terrestrial material directly in the laboratory. Observations of the diffuse interstellar medium (DISM) and molecular clouds (MC) set constraints on the composition of organic solids and large molecules, that! can then be compared with collected extraterrestrial materials analyses, to shed light on their possible links
Interstellar and interplanetary solids in the laboratory
International audienceThe composition of the interstellar matter is driven by environmental parameters (e.g. elemental abundance, density, reactant nature, radiations, temperature, time scales) and results also from external interstellar medium physico-chemical conditions. Astrochemists must rely on remote observations to monitor and analyze the comÂposition of interstellar solids. These observations give essentially access to the molecular functionality of the solids, rarely elemental composition constraints and isotopic fractionation only in the gas phase. Astrochemists bring additional information from the study of analogues produced in the laboratory, placed in simulated space environments. Planetologists and cosmochemists can have access and spectroscopically examine collected extra-terrestrial material directly in the laboratory. Observations of the diffuse interstellar medium (DISM) and molecular clouds (MC) set constraints on the composition of organic solids and large molecules, that! can then be compared with collected extraterrestrial materials analyses, to shed light on their possible links
Rearrangement of valence neutrons in the neutrinoless double-\beta decay of 136Xe
A quantitative description of the change in ground-state neutron occupancies
between Xe and Ba, the initial and final state in the
neutrinoless double- decay of Xe, has been extracted from
precision measurements of the cross sections of single-neutron adding and
-removing reactions. Comparisons are made to recent theoretical calculations of
the same properties using various nuclear-structure models. These are the same
calculations used to determine the magnitude of the nuclear matrix elements for
the process, which at present disagree with each other by factors of 2 or 3.
The experimental neutron occupancies show some disagreement with the
theoretical calculations.Comment: 7 pages, 3 figures, 1 tabl
First Exploration of Neutron Shell Structure below Lead and beyond N=126
The nuclei below lead but with more than 126 neutrons are crucial to an understanding of the astrophysical r process in producing nuclei heavier than AâŒ190. Despite their importance, the structure and properties of these nuclei remain experimentally untested as they are difficult to produce in nuclear reactions with stable beams. In a first exploration of the shell structure of this region, neutron excitations in 207Hg have been probed using the neutron-adding (d,p) reaction in inverse kinematics. The radioactive beam of 206Hg was delivered to the new ISOLDE Solenoidal Spectrometer at an energy above the Coulomb barrier. The spectroscopy of 207Hg marks a first step in improving our understanding of the relevant structural properties of nuclei involved in a key part of the path of the r process.peerReviewe