Nuclear Liquid-Drop Model Applied to Radioactive Decay Modes

2020 ◽  
Vol 29 (05) ◽  
pp. 2050028 ◽  
Author(s):  
H. C. Manjunatha ◽  
N. Sowmya ◽  
N. Manjunath ◽  
L. Seenappa

It was recognized that the magic numbers of nuclei 2, 20, 28, 50, 82 and 126 are predicted to be more stable than the neighbor nuclei. Later on the researchers predicted that the magic numbers for protons are 114, 122, 124 and 164 and the magic numbers for neutrons are 184, 196, 236 and 318. The predicted second generation magic number for proton and neutron comes in the superheavy nuclei region. The superheavy nuclei with magic number of protons/neutrons are [Formula: see text]114, [Formula: see text]114, [Formula: see text]122, [Formula: see text]122, [Formula: see text]124, [Formula: see text]124, [Formula: see text]126 and [Formula: see text]126. All the possible decay modes have been studied by using three different models such as modified generalized liquid drop model, dynamical cluster model and coulomb-proximity potential model. In the second part of this study, we have made detailed investigations to synthesize the above said nuclei using fusion reactions with modified Woods–Saxon potential model. This study also identifies the most possible projectile target combinations for the synthesis of the predicted magic nuclei in the superheavy nuclei region.


1963 ◽  
Vol 46 ◽  
pp. 639-659 ◽  
Author(s):  
V.M. Strutinsky ◽  
N.Ya. Lyashchenko ◽  
N.A. Popov

1999 ◽  
Vol 652 (2) ◽  
pp. 142-163 ◽  
Author(s):  
J. Piperova ◽  
D. Samsoen ◽  
P. Quentin ◽  
K. Bencheikh ◽  
J. Bartel ◽  
...  

Author(s):  
Rupert L. Frank ◽  
Phan Thành Nam

AbstractWe revisit the liquid drop model with a general Riesz potential. Our new result is the existence of minimizers for the conjectured optimal range of parameters. We also prove a conditional uniqueness of minimizers and a nonexistence result for heavy nuclei.


2021 ◽  
Vol 2103 (1) ◽  
pp. 012004
Author(s):  
N A Zemlyakov ◽  
A I Chugunov ◽  
N N Shchechilin

Abstract Neutron stars are superdense compact astrophysical objects. The central region of the neuron star (the core) consists of locally homogeneous nuclear matter, while in the outer region (the crust) nucleons are clustered. In the outer crust these nuclear clusters represent neutron-rich atomic nuclei and all nucleons are bound within them. Whereas in the inner crust some neutrons are unbound, but nuclear clusters still keeps generally spherical shape. Here we consider the region between the crust and the core of the star, so-called mantle, where non-spherical nuclear clusters may exist. We apply compressible liquid drop model to calculate the energy density for several shape types of nuclear clusters. It allows us to identify the most energetically favorable configuration as function of baryon number density. Employing four Skyrme-type forces (SLy4 and BSk24, BSk25, BSk26), which are widely used in the neutron star physics, we faced with strong model dependence of the ground state composition. In particular, in agreement with previous works within liquid drop model, mantle is absent for SLy4 (nuclear spheres directly transit into homogeneous nuclear matter; exotic nuclear shapes do not appear).


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