Direct counterfactual transmission of a quantum state

Evolution of collective structures in the heavy transitional nuclei above the N = 82 closed shell

“…3(a) and 3(b) shows that band 1 in 162 W has a lower alignment gain than band 1 in its heavier even-mass neighbour, 164 W. Gamma-ray spectroscopy studies of N < 90 nuclei suggest that the low average deformation of these nuclei favours excitations involving the negative-parity (ν f 7/2 , νh 9/2 ) states [10,[34][35][36][37][38]. The quadrupole deformation of 164 W is predicted be larger (β 2 = 0.161) than 162 W (β 2 = 0.116) [39], which is sufficient to bring the lowest Ω νi 13/2 orbital close to the Fermi surface.…”

The Trojan Horse Method as a tool for investigating astrophysically relevant fusion reactions

“…The data show a remarkable difference in the depletion result of beryllium at different stellar masses, being this the combined effect of both stellar structure and metallicity of the adopted models. As matter of example, models of solar metallicity with masses of about 0.08≤M/M ≤0.5 with effective temperatures 2600-3600 K show a maximum difference of the 9 Be logarithmic abundance of more than 1 dex when using the THM 9 Be(p,α) 6 Li reaction rate instead of the NACRE one [18].…”

“…In Eq. 2 the bare-nucleus S(E)-factor, S b (E), is the one Figure 1: Left panel: The 9 Be(p,α) 6 Li S(E)-factor as given by the THM measurements [20] (black points) compared with the direct measurements available in the NACRE compilation [21]. The full line represents the bare-nucleus THM S(E)-factor while the dashed one refers to its enhancing with the extracted U e =676±86 eV [20].…”

“…However, the comparison between the THM reaction rate and the one proposed in the widely used NACRE compilation [21] leads to a ∼20% of discrepancy, thus calling for an evaluation of the impact of the THM reaction rate in astrophysical environments. Besides the role played by deuteron, lithium-7 and lithium-6 abundances already investigated in [25][26][27][28], the THM 9 Be(p,α) 6 Li S(E)-factor measurements have been then used in [18] for evaluating the fate of 9 Be in pre-main sequence (PMS) stars by means of the PROSECCO stellar code derived from the well tested FRANEC one [22,23]. The calculations have been performed in a wide stellar mass range, starting from 0.08 M up to 0.7 M for different stellar ages and metallicity.…”

“…In the last work of [18], the impact of the THM measurements for the (p,α) cross sections involving 9 Be and 10 B has been evaluated. In particular, the 9 Be(p,α) 6 Li THM measurement has been firstly investigated in [19] while an improved measurement is given in [20]. The latter one has been used to firstly extract the bare-nucleus S b (E)-factor and then for calculating the corresponding reaction rate, by means of standard formulas (see [18] for details).…”