Alpha-cluster preformation factor within cluster-formation model for odd-A and odd–odd heavy nuclei

The accurate calculations of the cluster formation model (CFM) have been extended to determine the alpha cluster preformation probability for the three even–even superheavy isotopes (Hs, Ds and Cn) with atomic number [Formula: see text] and 112 and neutron numbers [Formula: see text] in the mass region from 252 to 300. According to the hypothesized CFM, the calculations of the formation energy and surface energy, which depended on differences of binding energies are crucial for determining the realistic values of the preformation probability. Our results showed reasonable agreement with the results of previous work for the heavy nuclei. In addition, realistic values of the preformation probability certified that CFM can successfully be used to calculate the alpha cluster preformation probability for other wide range of superheavy nuclei.

Download Full-text

Erratum: Alpha-cluster preformation factors in alpha decay for even–even heavy nuclei using the cluster-formation model

Journal of Physics G Nuclear and Particle Physics ◽

10.1088/0954-3899/40/7/079601 ◽

2013 ◽

Vol 40 (7) ◽

pp. 079601 ◽

Cited By ~ 5

Author(s):

Saad M Saleh Ahmed ◽

Redzuwan Yahaya ◽

Shahidan Radiman ◽

Muhamad Samudi Yasir

Keyword(s):

Cluster Formation ◽

Alpha Decay ◽

Heavy Nuclei ◽

Formation Model ◽

Alpha Cluster

Download Full-text

Alpha-cluster preformation factors in alpha decay for even–even heavy nuclei using the cluster-formation model

Journal of Physics G Nuclear and Particle Physics ◽

10.1088/0954-3899/40/6/065105 ◽

2013 ◽

Vol 40 (6) ◽

pp. 065105 ◽

Cited By ~ 27

Author(s):

Saad M Saleh Ahmed ◽

Redzuwan Yahaya ◽

Shahidan Radiman ◽

Muhamad Samudi Yasir

Keyword(s):

Cluster Formation ◽

Alpha Decay ◽

Heavy Nuclei ◽

Formation Model ◽

Alpha Cluster

Download Full-text

The globular cluster system of the Auriga simulations

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1380 ◽

2020 ◽

Vol 496 (1) ◽

pp. 638-648 ◽

Cited By ~ 1

Author(s):

Timo L R Halbesma ◽

Robert J J Grand ◽

Facundo A Gómez ◽

Federico Marinacci ◽

Rüdiger Pakmor ◽

...

Keyword(s):

Globular Cluster ◽

Milky Way ◽

Cluster Formation ◽

Solar Radius ◽

High Mass ◽

Formation Model ◽

The Galaxy ◽

High Mass Loss ◽

Globular Cluster System ◽

Varying Mass

ABSTRACT We investigate whether the galaxy and star formation model used for the Auriga simulations can produce a realistic globular cluster (GC) population. We compare statistics of GC candidate star particles in the Auriga haloes with catalogues of the Milky Way (MW) and Andromeda (M31) GC populations. We find that the Auriga simulations do produce sufficient stellar mass for GC candidates at radii and metallicities that are typical for the MW GC system (GCS). We also find varying mass ratios of the simulated GC candidates relative to the observed mass in the MW and M31 GCSs for different bins of galactocentric radius metallicity (rgal–[Fe/H]). Overall, the Auriga simulations produce GC candidates with higher metallicities than the MW and M31 GCS and they are found at larger radii than observed. The Auriga simulations would require bound cluster formation efficiencies higher than 10 per cent for the metal-poor GC candidates, and those within the Solar radius should experience negligible destruction rates to be consistent with observations. GC candidates in the outer halo, on the other hand, should either have low formation efficiencies, or experience high mass-loss for the Auriga simulations to produce a GCS that is consistent with that of the MW or M31. Finally, the scatter in the metallicity as well as in the radial distribution between different Auriga runs is considerably smaller than the differences between that of the MW and M31 GCSs. The Auriga model is unlikely to give rise to a GCS that can be consistent with both galaxies.

Download Full-text

Formation of α clusters in dilute neutron-rich matter

Science ◽

10.1126/science.abe4688 ◽

2021 ◽

Vol 371 (6526) ◽

pp. 260-264 ◽

Cited By ~ 1

Author(s):

Junki Tanaka ◽

Zaihong Yang ◽

Stefan Typel ◽

Satoshi Adachi ◽

Shiwei Bai ◽

...

Keyword(s):

Cross Sections ◽

Cluster Formation ◽

Reaction Cross ◽

Skin Thickness ◽

Neutron Skin ◽

Heavy Nuclei ◽

Α Decay ◽

Neutron Skin Thickness ◽

Reaction Cross Sections ◽

Α Particles

The surface of neutron-rich heavy nuclei, with a neutron skin created by excess neutrons, provides an important terrestrial model system to study dilute neutron-rich matter. By using quasi-free α cluster–knockout reactions, we obtained direct experimental evidence for the formation of α clusters at the surface of neutron-rich tin isotopes. The observed monotonous decrease of the reaction cross sections with increasing mass number, in excellent agreement with the theoretical prediction, implies a tight interplay between α-cluster formation and the neutron skin. This result, in turn, calls for a revision of the correlation between the neutron-skin thickness and the density dependence of the symmetry energy, which is essential for understanding neutron stars. Our result also provides a natural explanation for the origin of α particles in α decay.

Download Full-text