Abstract
The~Space Star Anomaly in proton-deuteron breakup cross-section occurs at energies of about 10~MeV. Data for higher energies are sparse. Therefore, a~systematic scan over star configurations in the~range of intermediate energies between 50 and 100 MeV/nucleon is carried out on the~basis of data collected with the~large acceptance BINA detector. The~preliminary cross section results for forward star configurations at 80 MeV/nucleon slightly surpass the~theoretical calculations, but the~systematic uncertainties are still under study. Also, a~new variable describing rotation of star configurations is proposed.
Highlights
Studies of the most basic properties of nuclear interactions require a system simple enough for the strict calculations to be performed, which at the same time should be complicated enough to make some additional dynamics possible
The experiments performed with Big Instrument for Nuclear Polarization Analysis (BINA) at KVI, Groningen, and the ongoing measurements at Cyclotron Centre Bronowice (CCB), Krakow, make possible to extend the experimental data on the Space Star cross section at 50, 80, 108 and 160 MeV/nucleon
The angle α=20◦ corresponds to polar angles of registered protons θ1=θ2=24.2◦±1◦ and relative azimuthal angle φ12=157.7◦±5◦; α=40◦ corresponds to θ1=θ2=26.3◦±1◦ and φ12=139.3◦±5◦; α=60◦ corresponds to θ1=θ2=29.2◦±1◦ and φ12=126.9◦±5◦
Summary
Studies of the most basic properties of nuclear interactions require a system simple enough for the strict calculations to be performed, which at the same time should be complicated enough to make some additional dynamics possible. Phenomenological NN potentials are either complemented with additional diagrams treating excitations on an equal footing with nucleons, as if stable particles were produced (∆-isobar in Coupled Channels approach) or with a phenomenological 3NF model Another approach is more fundamental and applies the Chiral Perturbation Theory in order to reach an EFT description (Chiral EFT) [1, 2]. The most intriguing inconsistencies are the Ay puzzle (for analysing powers) and the Space Star Anomaly (SSA) observed in the differential cross-section of the breakup reaction. The latter effect is surprising, as it occurs at relatively low energies. The only published data about the Space Star for this energy range showed lack of the effect for 65 MeV [10], while for the second highest energy (19 MeV) the effect was small, but still visible [11]
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