This study provides a comprehensive examination of the surface properties—particularly the symmetry energy and its contributing components—of isotonic chains across various mass ranges, including light, medium, heavy, and superheavy nuclei. We establish a correlation between nuclear symmetry energy and isospin asymmetry in different mass regions along isotonic chains with magic and semi-magic neutron numbers of N = 20, 40, 82, 126, and 172. Our approach integrates the coherent density fluctuation model within the relativistic mean-field (RMF) framework, utilizing both the non-linear NL3 and density-dependent DD-ME2 parameter sets. The methodology employs the Brueckner energy density functional in conjunction with our recently developed relativistic energy density functional (relativistic-EDF). The relativistic parameterization of the EDF at local density facilitates a consistent exploration of isospin-dependent surface properties across the nuclear landscape. In the present work, we successfully reproduce established shell closures and demonstrate that the relativistic approach yields significantly improved predictions for recognized magic numbers, particularly Z = 28 and 50. Additionally, we present compelling evidence for the presence of novel shell and sub-shell closures, specifically at Z = 34, 58, 92, and 118. These findings contribute to a nuanced understanding of nuclear surface properties while serving as a benchmark for future investigations and validations of nuclear models.

In the present work, we have incorporated the microscopic relativistic nuclear potential obtained from recently developed relativistic R3Y NN potential in the coupled channels code CCFULL to study the fusion dynamics. The R3Y NN-potential and the densities of interacting nuclei are obtained for the relativistic mean-field approach for the NL3$^*$ parameter set. It is to be noted that the R3Y NN potential can be expressed in terms of masses of the mesons and their couplings by considering the meson degrees of freedom within the relativistic mean field, which has a form similar to the widely used M3Y potential. We focused on the fusion cross-sections for $Oxygen$-based reactions with targets from different mass regions of the periodic table i.e. $^{16}$O + $^{24}$Mg, $^{18}$O + $^{24}$Mg, $^{16}$O + $^{148}$Sm, $^{16}$O + $^{176}$Hf, $^{16}$O + $^{176}$Yb, $^{16}$O + $^{182}$W, and $^{16}$O + $^{186}$W. A comparison is also made with the ones calculated using the nuclear potential obtained from the traditional Woods-Saxon potential and the widely used M3Y NN potential within CCFULL. The coupled channel calculations are performed with shape and rotational degrees of freedom to examine the fusion enhancement at below-barrier energies. It is observed from the calculations that the fusion cross-sections obtained using R3Y NN potential with rotational degrees of freedom are found to be more consistent with the experimental data than those for the M3Y and Woods-Saxon potentials mainly at below barrier energies.

The neutron skin of atomic nuclei impacts the structure of neutron-rich nuclei, but its accurate measurement is quite challenging. We present predictions for neutron skins and proton radii for light to medium mass nuclei by employing Covariant Density Functional Theory (CDFT) based on density-dependent meson-exchange interaction. Using our microscopic predictions, we find a linear correlation between the neutron skin and the isospin asymmetry. The calculations are also extended to find a linear relationship between proton and neutron radii of mirror nuclei. Using the charge symmetry property of nuclear forces, a correlation between the neutron skin of neutron-rich nuclei and difference between the proton radii of the corresponding mirror pair has also been investigated. The inclusion of ISB term is found to affect the mirror difference charge radii of [Formula: see text]Ca-[Formula: see text]Ni mirror pair.

The cluster dynamics of radioactive nuclei decaying to neighbouring daughter nuclei of the double magic ^132 Sn and ^208 Pb is investigated using the relativistic mean-field (RMF) approach with NL3 ^* parameter set within the preformed cluster-decay model (PCM). The novel feature of the present study is the application of the newly derived preformation formula, laying the groundwork for accessing the break-up of the Q-value: preformation energy, cluster emission energy and the recoil energy of the daughters formed. The energy associated with cluster preformation is theoretically quantified for the first time. This treatment underscores the shell effect, pairing correlation, and blocking of particular orbitals by unpaired nucleons. To ascertain the applicability of the new formula, PCM-based calculations are carried out with nuclear potential obtained using the phenomenological M3Y and microscopic RMF-based R3Y nucleon-nucleon (NN) potentials along with the corresponding densities. We observed a slight discrepancy attributable to differences in their barrier properties. Nonetheless, predictions using both M3Y and R3Y potentials align well with experimental half-lives. While none of the reaction systems resulted in a double magic daughter nucleus, we observed that the kinematics of cluster emissions are influenced by their proximity to shell closures. Analyzing the systematic recoil energy in cluster decays offers valuable insights for synthesizing elements in superheavy mass regions in the future.

In the present work, we constrain the equations of the state of asymmetric dense matter in consideration of the heaviest observed neutron star mass M _max = 2.35± 0.17 M _⊙ for the black widow pulsar PSR J0952-0607, finite and bulk nuclear properties. We propose four interactions for the relativistic mean field model which include different combinations of non-linear, self, and cross-couplings among isoscalar–scalar σ , isoscalar–vector ω , isovector–vector ρ and isovector–scalar meson δ meson fields up to the quartic order. These interactions harmonize with the finite nuclei and bulk nuclear matter properties. It is observed that interactions obtained with the inclusion of δ meson coupling with nucleons have a significant effect on the slope of symmetry energy (L), radius (R _1.4), and dimensionless tidal deformability ( _1.4) corresponding to a canonical mass neutron star. The radius of 2.08M_⊙ neutron star mass is predicted to be in the range R_2.08 = 12.98–13.34 km which also satisfies the NICER observations Miller et al. (Astrophys. J. Lett. 918, L28 (2021).

We investigated the effect of the degree of freedom of neutron transfer on the cross section of heavy-ion fusion reactions, using the relativistic mean-field formalism within the coupled-channels approach (CCFULL). We obtain the microscopic nuclear interaction potential in terms of the density distributions for the targets and projectiles with the NL3 & lowast; parameter set and corresponding R3Y nucleon-nucleon potential. The present analysis includes the 18O-induced reactions, namely, 18O + 58,60,64Ni, 18O + 74Ge, 18O + 148Nd, 18O + 150Sm, and 18O + 182,184,186W for which experimental fusion cross sections are available around the Coulomb barrier. It is evident from the results that including vibrational and/or rotational degrees of freedom enhances the fusion cross section at energies below the barrier. However, fusion hindrance persists in this energy region. To address this, we incorporated the two-neutron (2n) transfer channels in the coupled-channels calculation. A comparison with the Woods-Saxon (WS) potential shows that the R3Y nucleon-nucleon (NN) potential, with intrinsic degrees of freedom, is superior to it, especially at energies below the barrier. This superiority can be attributed to the observed higher barrier heights and lower cross section of the WS potential compared to the relativistic R3Y NN potential for the considered reaction systems. Consequently, we employed the relativistic mean-field formalism to estimate fusion characteristics for the unknown 18O-induced reactions, namely 18O + 62Ni, 18O + 70,72,76Ge, 18O + 144,150Nd, and 18O + 144,148,152,154Sm. Our analysis highlights the significant role of positive Q-value neutron transfer in enhancing the sub-barrier fusion cross section for the 18O + 148Nd reaction with the R3Y NN potential. However, the effect of this transfer channel for the other considered reactions is comparatively less pronounced.

Nuclear shape and orientation degrees of freedom are incorporated into the calculation of the double-folding nuclear potential within the relativistic mean-field (RMF) formalism. The quadrupole deformations (beta 2), beta 2 ), nuclear densities, and the effective nucleon-nucleon (NN) NN ) interaction potential are obtained using the RMF approach for the hybrid, NL3 & lowast;, & lowast; , and NL3 parametrizations. The calculated quadrupole deformations are included in the target densities through the nuclear radius. The deformation and orientation-dependent microscopic nuclear potentials are further employed to obtain fusion barrier characteristics and cross sections for 12 even-even heavy-ion reactions with doubly magic spherical 16O O and 48 Ca as projectiles along with deformed targets from different mass regions. The results obtained for the relativistic R3Y NN potential are compared with those of the Reid version of the nonrelativistic M3Y NN potential as well as with the available experimental data. A decrease in the barrier height and increase in the cross-section is observed upon the inclusion of target quadrupole deformations in the nuclear density distributions at the target orientation angles, 0 2 58 degrees degrees for the R3Y NN potential and at 0 2 60 degrees degrees for the M3Y NN potential. On comparing the 0 2-integrated cross section calculated using M3Y and R3Y NN potentials with spherical and deformed densities, one observes that the deformed densities and the relativistic R3Y NN potential obtained for the hybrid parameter set provide better agreement with the available experimental data for all the considered reactions. Moreover, the modifications in the characteristics of the fusion barrier and hence in the cross section with the inclusion of nuclear shape degrees of freedom and orientations are found to become more prominent in reactions forming heavier compound nuclei. This implies that the inclusion of nuclear deformations and orientation in the calculation of the microscopic nuclear potential within the RMF formalism is crucial to provide a reliable description of the sub-barrier nuclear fusion dynamics, especially in the heavy and superheavy mass regions.

The recently precise parity-violating electron scattering experiments CREX and PREX-II results on neutron skin thickness for 48Ca and 208Pb nucleus suggest a distinctive picture of linear density dependence of symmetry energy (L) and equation of state (EoS) of dense nuclear matter. The PREX-II results demand a large value of L, suggesting stiffer EoS, whereas CREX results support small L and softer EoS. This discrepancy has caused large tension among theoretical, experimental, and observational groups to reproduce the ground state properties of finite nuclei, simultaneously satisfying the CREX-PREX results and properties of neutron stars within the astrophysical observations. Motivated by this, we propose the interactions for the relativistic mean field (RMF) model by taking into account the coupling of isovector scalar 8 meson-nucleon (g8), cubic (Q82) and quartic order interactions ( r282) due to isoscalar scalar a and isovector scalar, 8 mesons, in addition to vector meson mixing w2 rho 2. These interactions reproduce the binding energies and charge radii of spherical/closed shell nuclei and also satisfy the CREX and PREX-II results on neutron skin thickness for 48Ca and 208Pb nucleus and give a plausible solution to the CREX-PREX-II dilemma. It is also observed that for the RMF model to satisfy the CREX-PREX-II constraints simultaneously, L should lie in the range 79.32 +/- 6.20 MeV. The equations of state composed of /3-equilibrated nucleonic matter obtained for these interactions are very stiff. The prediction of nuclear matter and neutron star observables for these interactions are also discussed.

The structure of target and projectile nuclei can significantly affect the reaction dynamics at low energies. In the present work, the fusion mechanism of Ni-58,Ni-64+Mo-92,Mo-100 reactions involving the Mo isotopes exhibiting peculiar soft nature is explored within the relativistic mean-field (RMF) formalism. The cross-section for the considered reactions is obtained using the l-summed Wong model furnished with nuclear interaction potential calculated within the self-consistent RMF formalism. The calculations are done for the two sets of RMF parameters, namely, NL3* and NL1, which give different values for various characteristics of nuclear matter at the saturation. A lower fusion barrier and consequently, a higher cross-section is obtained for the parameter set with comparatively softer equation of state (EoS). On comparing the theoretical cross-section with the available experimental data, an underestimation of fusion cross-section with respect to the experimental data at the sub-barrier energies is noted for the NL3* parametrizations. The match improves for the NL1 set having soft EoS with slight underestimation of data noted for all the considered reactions. These observations infer that the incomprehensible softness of Mo-isotopes also persists in their fusion dynamics, and the nuclear potential obtained within the RMF formalism is observed to underestimate the fusion probability for the reactions involving Mo-isotopes. The compressible nature of Mo-isotopes is inferred to enhance the fusion cross-section, and nuclear potential obtained for parameter set with soft EoS is observed to be more suitable for the description of their fusion dynamics.

The influence of nuclear rotation on the decay half-lives of superheavy nuclei within the range 98≤Z≤120 is investigated using the axially deformed relativistic Hartree-Bogoliubov theory in the continuum (DRHBc) with the PC-PK1 parameter set. The deduced DRHBc decay energies (with and without the rotation effect) are compared with those calculated from the macroscopic-microscopic WS4 and the available experimental binding energies. Six semi-empirical formulae, such as the Viola-Seaborg formula (VSS), the modified Brown formula (mB1), the semi-empirical relationship based on fission theory (SemFIS2), the Royer formula (R), the Wang formula (Wang) and the modified YQZR formula (MYQZR) are employed to estimate the half-lives of α decay. Among these formulae, the half-live predictions of SemFIS2 are found to gradually deviate from the systematic trend beyond Nd=184, showing that the probability of undergoing spontaneous fission is less feasible beyond this point. A minimum is observed at Nd=184, reflecting its neutron shell closure for the mass region considered on the nuclear chart. The results further indicate that, for 98≤Z≤104, the predictions of all semi-empirical formulae are more closely matched to the available experimental data when the rotation effect is taken into account. However, we have demonstrated that the effect of nuclear rotation gradually reduces as the atomic nucleus becomes heavier.

In this theoretical study, we have derived a simplified analytical expression for the binding energy per nucleon as a function of density and isospin asymmetry within the relativistic mean-field model. We have generated a new parameterization for the density-dependent DD-ME2 parameter set using the Relativistic-Hartree-Bogoliubov approach. Moreover, this work attempts to revisit the prior polynomial fitting in KUMAR A. et al., Phys. Rev. C, 103 (2021) 024305 for the non-linear NL3 force parameter to provide a simplified set of equations for the energy density functional which is used for calculating the surface properties of finite nuclei. The current study improves the existing fitting procedure by effectively proposing a simpler model that provides comparably precise results while lowering the computational expense. To study the surface properties of finite nuclei with these parameterizations, we have adopted the coherent density fluctuation model, which effectively translates the quantities of nuclear matter from momentum space to coordinate space at local density. The isospin properties, such as symmetry energy and its surface and volume components, slope parameter, finite nuclear incompressibility, and surface incompressibility for even-even nuclei, are calculated for different mass regions. Moreover, we have studied the effect of density, weight function, and choice of relativistic force parameters on the surface properties. The significance of this work will help to determine the properties of nuclei along the nuclear landscape and can facilitate an improved understanding of the island of stability, heavy-ion collision, and nucleosynthesis, among others. Copyright (c) 2024 EPLA

The fusion mechanism of reactions involving even-even 112-124Sn, doubly magic 132Sn, 208Pb as targets, and 64Ni as the projectile is explored within the relativistic mean field (RMF) formalism. The main aim of choosing these nuclei is to explore the correlation between the nuclear incompressibility and the fusion cross section. The nucleus-nucleus interaction potential is calculated by folding the axially deformed nuclear densities and the relativistic R3Y nucleon-nucleon (NN) potential obtained for the nonlinear NL3 & lowast;, hybrid, and NL1 parameter sets, which yield different values for various characteristics of nuclear matter at saturation. The fusion barrier characteristics obtained for different RMF parametrizations are further used to calculate the cross section within the -summed pound Wong model. We found a decrease in the barrier height and, consequently, an increase in the cross section with a decrease in the incompressibility for all sets of parameters considered. Furthermore, comparing the barrier heights obtained for NL3 & lowast; and the hybrid parameters, it is observed that the barrier height decreases with decreasing symmetric energy and incompressibility value. Moreover, a lower barrier height and, consequently, a higher cross section at below-barrier energies is observed for the NL1 parameter set, which gives a soft equation of state (EoS) having a lower value of nuclear matter incompressibility. The calculated cross section is satisfactorily consistent with the available experimental data for 64Ni +208Pb system. In contrast, the nuclear potentials obtained for NL3 & lowast; and hybrid parameter sets underestimate the cross section at below-barrier energies for 64Ni + 112-124,132Sn reactions. This discrepancy between the experimental data and the theoretical results for 64Ni + 112-124,132Sn reactions can be correlated with the soft behavior of the Sn isotopes. The compressible nature of Sn isotopes is inferred to lower the barrier height, which further leads to enhancement of the experimental fusion and/or capture cross section at below-barrier energies. Thus, the NL1 parameter set with a comparatively soft EoS is observed to be a better choice to describe the sub-barrier nuclear fusion dynamics of reactions involving the Sn isotopes.

In the present work, we investigate the bulk properties of nuclear matter and neutron stars with the newly proposed relativistic interaction NL-RS which provides an opportunity to readjust the coupling constants keeping in view the properties of finite nuclei, nuclear matter, PREX-II results for neutron skin thickness in 208Pb and astrophysical observations. The NL-RS model interaction has been proposed by fitting the ground state properties (binding energies and charge radii) of finite nuclei, bulk nuclear matter properties, and PREX-II results for neutron skin thickness of 208Pb. The relativistic interaction has been generated by including nonlinear self-interactions of sigma and omega mu -mesons and mixed interactions of omega mu , and rho mu -meson up to the quartic order. The proposed interaction harmonizes with the finite nuclei, bulk nuclear matter, and neutron star properties. A covariance analysis is performed to assess the statistical uncertainties on the model parameters and nuclear observables of interest along with correlations amongst them. The equation of state (EoS) composed of nucleons and leptons in beta-equilibrium is computed with the proposed parameter set and used to study the neutron star structure. The maximum mass of the neutron star by employing the EoS computed with the NL-RS parameter set is 2.04 +/- 0.03M circle dot and the radius of a canonical mass neutron star (R 1.4) comes out to be equal to 13.06 +/- 0.16 Km. The value of dimensionless tidal deformability, for canonical mass, is 602.23 +/- 33.13 which satisfies the constraints of waveform models analysis of GW170817 within 90% confidence level.

The quadrupole (β2) deformed targets in the actinide region are found to be of great relevance in the production of superheavy nuclei (SHN), in the compact fusion mechanism. Recently, the application of “elongated” and “compact” configurations of pear-shape octupole (up to β3) deformed nuclei was found to play a significant role in the fusion-fission dynamics of heavy-ion induced reactions. In the present work, we intend to explore the relevance of higher-order deformed (up to β4) actinides and their compact configuration in the production cross-section as well as de-excitation of SHN (dynamics of 48Ca + 238U →286Cn∗ → A1 + A2 reaction). For the above analysis, we have calculated σER within the framework of dynamical cluster-decay model developed on the basis of quantum mechanical fragmentation theory, which has been extended with the inclusion of deformations up to β4 and corresponding compact optimum orientation. Besides, on the basis of this theory, the fragmentation structure of 286Cn∗ superheavy nucleus is examined in terms of fragmentation potential (Vη) and preformation probability (P0) as a function of fragment mass number.

The α -decay half-lives of superheavy nuclei with 100 ⩽ Z ⩽ 120 are comprehensively analyzed using the axially deformed relativistic mean field (RMF) formalism for the NL3* parameter set. We employ RMF binding energies to determine the α -decay energies and make a comparison with both the available experimental data and the theoretical results obtained from the global nuclear mass model WS4. The four distinct formulae, specifically the modified scaling law Brown, modified Viola-Seaborg, Yibin et al. formula, and its modified form are used to calculate the decay half-lives and examine the numerical correlation between the half-life ( T_1/2 ) for each α -decay energy. We notice that T_1/2 is significantly dependent on the decay formula in terms of isospin asymmetry and decay energy. We also noticed that modified scaling law Brown formula estimates of half-lives agreed comparatively better with the experiment as compared to others. Moreover, the present investigation provides significant information on the stability of the superheavy island considered for ongoing and/or future experiments.

The cluster dynamics of radioactive nuclei decaying to neighbouring daughter nuclei of the double magic $^{132}$Sn and $^{208}$Pb is investigated using the relativistic mean-field (RMF) approach with NL3$^*$ parameter set within the preformed cluster-decay model (PCM). The novel feature of the present study is the application of the newly derived preformation formula, laying the groundwork for accessing the break-up of the Q-value: preformation energy, cluster emission energy and the recoil energy of the daughters formed. The energy associated with cluster preformation is theoretically quantified for the first time. This treatment underscores the shell effect, pairing correlation as well as the blocking of particular orbitals by unpaired nucleons. To ascertain the applicability of the new formula, the PCM based calculations are carried out with nuclear potential obtained using the phenomenological M3Y and microscopic RMF-based R3Y nucleon-nucleon (NN) potentials along with corresponding densities. We found a marginal variation that can be attributed to the difference in their barrier properties, however, the predictions for the case of both M3Y and R3Y potentials are found to agree well with the experimental half-lives. Although none of the considered reaction systems yields a double magic daughter nucleus, we found that the kinematics of their cluster emissions is governed by their proximity to the shell closure. The deduced systematic of the recoil energy in cluster decays can provide valuable insight for the synthesis of elements in superheavy mass region in the future.

The analytical expression of the density-dependent binding energy per nucleon for the relativistic mean field (RMF), also known as the relativistic energy density functional (Relativistic-EDF), is used to obtain the isospin-dependent symmetry energy and its components for the isotopic chain of Sc, Ti, V, and Cr nuclei. The procedure of the coherent density fluctuation model is employed to formulate the Relativistic-EDF and Brueckner energy density functional (Brueckner-EDF) at local density. A few signatures of shell and/or sub-shell closure are observed in the symmetry energy and its components, i.e., surface and volume symmetry energy, far from the beta-stable region for odd-A Sc and V, and even-even Ti and Cr nuclei with non-linear NL3 and G3 parameter sets. A comparison is made with the results obtained from Relativistic-EDF and Brueckner-EDF with both NL3 and G3 for the considered isotopic chains. We find Relativistic-EDF outperforms the Brueckner-EDF in predicting the shell and/or sub-shell closure of neutron-rich isotopes at N = 50 for these atomic nuclei. Moreover, a relative comparison has been made for the results obtained with the non-linear NL3 and G3 parameter sets.

The bulk properties of nuclear matter and neutron stars with the newly generated relativistic interaction Dev Bhoomi Himachal Pradesh (DBHP) are investigated, which provides an opportunity to modify the coupling parameters keeping in view the finite nuclei, nuclear matter, PREX-II data for neutron skin thickness in 208Pb, and astrophysical constraints. The relativistic interaction has been generated by including all possible self and mixed interactions among sigma, omega, and rho mesons up to the quartic order satisfying the naturalness behavior of parameters. A covariance analysis is performed to assess the statistical uncertainties of the model parameters and observables of interest along with correlations amongst them. We obtained a value of neutron skin thickness for the 208Pb nucleus of Delta rnp = 0.24 +/- 0.02 fm. The maximum gravitational mass of a neutron star and the radius corresponding to the canonical mass (R1.4) come out to be 2.03 +/- 0.04 Mo and 13.39 +/- 0.41 km, respectively. The dimensionless tidal deformability A for a neutron star is also analyzed.

In the present work, we constrain the equation of the state of dense matter in the context of heaviest observed neutron star mass M$_{max}$ = 2.35$\pm 0.17$ M$_{\odot}$ for the black widow pulsar PSR J0952-0607. We propose three interactions HPU1, HPU2 and HPU3 (named after Himachal Pradesh University)for the relativistic mean field model which include different combinations of non-linear, self and cross-couplings among isoscalar-scalar $\sigma$, isoscalar-vector $\omega$ and isovector-vector $\rho$ meson fields up to the quartic order. These interactions are in harmony with the finite nuclei and bulk nuclear matter properties. The equations of state computed by using newly generated interactions for the $\beta$-equilibrated nucleonic matter satisfy the heaviest observed neutron star mass M$_{max}$ = 2.35$\pm 0.17$ M$_{\odot}$ for the black widow pulsar PSR J0952-0607. The results for the radius ($R_{1.4}$) and dimensionless tidal deformability (${\Lambda_{1.4}}$) corresponding to the canonical mass are also presented and agree well with the GW170817 event and astrophysical observations. The radius of $2.08M_{\odot}$ neutron star mass is predicted to be in the range $R_{2.08}$ = 12.98 -13.09 Km which also satisfies the NICER observations by Miller et al. (2021) and Riley et al.(2021). A covariance analysis is also performed to assess the theoretical uncertainties of model parameters and to determine their correlations with nuclear matter observables.

The quadrupole ( β _λ =2 ) deformation and corresponding cold and hot optimum orientations of the nuclei play an important role in the synthesis of new nuclear entity. Consequently, a comprehensive knowledge is required to understand the relevance of higher-order deformed nuclei in the nuclear fusion dynamics. In the present work, the hexadecapole ( β _λ =2,4 ) deformed nuclei of different shapes, i.e. β _2^+β _4^+ ( ^147-150,152,154 Sm), β _2^+β _4^- ( ^172,174,176,178,180,182 Yb), β _2^-β _4^+ ( ^40,43,55,77,82 Sc) and β _2^-β _4^- ( ^70,72-74 Ge) are taken into consideration as target of ^16 O (sph.), ^48 Ca (sph.), ^48 Ar ( β _2^- ) and ^62 Fe ( β _2^+ ) induced reactions. For these selected choices of projectile-target (p-t) combinations, the impact of ± signs and hot/cold optimum orientations of higher-order deformation (up to β _4 ) has been investigated, in reference to that β _2^± deformation. The above analysis has been discussed in terms of fusion barrier characteristics (barrier height V_B and barrier position R_B ), which is sensitive towards the deformation and orientation degree of freedom. Furthermore, the corresponding effects have been analyzed in the calculation of fusion cross-section σ _fus , with respect to the center of mass energy ( E_c.m. ) lying across the Coulomb barrier. Therefore, the nuclear shape for targets β _2^±β _4^+ expands relatively larger, and consequently the radius which enhances the fusion cross-sectional area as compared to that of β _2^± deformation. In contrast to the above case, the β _2^±β _4^- shapes have been found to hinder the fusion, mainly at the below- and near-barrier regions. Subsequently, the present work gives the relevance of the expanded and compressed shapes of hexadecapole deformed nuclei in the nuclear fusion dynamics for the considered choices of p-t combinations at the low-energy regime. Besides, the available experimental data for ^16 O+ ^147-150,152,154 Sm p-t combinations, here ‘Sm’ isotopes are β _4^+ -deformed, has been addressed by integrating σ _fus over all orientations and deformations up to β _4 , over a given range of E_c.m. .