Study of hot thermally fissile nuclei using relativistic mean field theory
We have studied the properties of hot U and Pu nuclei in the frame-work of relativistic mean field formalism. The recently developed FSUGarnet and IOPB-I parameter sets are implemented for the first time to deform nuclei at finite temperature. The results are compared with the well known NL3 set. The said isotopes are structurally important because of the thermally fissile nature of U and Pu as these nuclei (U and Pu) are formed after the absorption of a thermal neutron, which undergoes fission. Here, we have evaluated the nuclear properties, such as shell correction energy, neutron-skin thickness, quadrupole and hexadecapole deformation parameters and asymmetry energy coefficient for these nuclei as a function of temperature.
Keywords: properties of nuclei, level density, single particle levels, symmetry energy, fission parameters
Out of 300 known stable nuclei in nature, the bottom part of the periodic table, known as actinide series, encompasses the elements from Z = 89 to 103 which have applications in smoke detectors, gas mantles, as a fuel in nuclear reactors and in nuclear weapon etc. Among the actinide, Thorium () and Uranium () are the most abundant elements in nature with their isotopic fraction: 100% of Th and 0.0054% U, 0.7204% U and 99.2742% U . The isotopes U and Pu are synthesized from Th and U, respectively by the bombardment of neutron and subsequent decay processes. These actinides are denser than Fe with hardness similar to that of soft steel. Apart from their hardness, the naturally occurred U and synthesized U and Pu breakdown immediately into fragments with the absorption of slow neutrons (zero energy neutrons or thermal neutrons). The isotopes U and Pu are quite stable in general as long as it is not disturbed by an almost zero energy external agent, such as a thermal neutron. Hence, these type of isotopes are called as the thermally fissile nuclei. These thermally fissile nuclei have a great importance for controlled energy production in nuclear reactors.
The nuclear fission is one of the most interesting phenomena from the time of its discovery by Otto Hahn and F. Strassmann in 1938 . When a thermally fissile nucleus, such as U or Pu absorbs a thermal neutron, it undergoes fission and releases nuclear energy, which is the main source of energy production in reactor technology. After forming the compound nucleus (U and Pu) it oscillates in different modes (quadrupole, hexadecapole) of vibrations and finally reaches to the scission point. In the process, the compound nucleus exhibits various stages including increase in temperature (T). To understand the fission dynamics, it is important to study the nuclear properties, like nuclear excitation energy , change in shapes and sizes of nucleus, variation of specific heat , effect of shell structure, change of single particle energy and inverse level density parameter. All these observables are crucial quantities to understand the fission phenomena and our aim is to analyze these properties with temperature.
Recently, the relative mass distribution of thermally fissile nuclei for binary  and ternary  fission processes are reported. Here, it is shown that the relative yield of fission fragments depend very much on the temperature of the system. The level density parameter is also influenced a lot with temperature, which is a key quantity in fission study. The neutron-skin thickness ( and are the root mean square radii of neutrons and protons distribution) has a direct correlation with the equation of state (EOS) of nuclear matter [5, 6]. It is to be noted that the neutron star EOS is the main ingredient which is used to predict the mass and radius of the star. The asymmetry energy coefficient is an important quantity for various nuclear properties, such as to establish proper boundaries for neutron and proton drip-lines, study of heavy ion collision, physics of supernovae explosions and neutron star [7, 8, 9]. Thus, it attracts the attention for the analysis of neutron-skin thickness and asymmetry energy coefficient as a function of temperature.
To study the fission process, a large number of models have been proposed [10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20]. The liquid drop model successfully explains the fission of a nucleus [19, 20, 21, 22] and the semi-empirical mass formula is the simple oldest tool to get a rough estimation of the energy released in a binary fission process. Most of the time, the liquid drop concept is applied to study the fission phenomenon, where the shell effect of the nucleus generally ignored. But, the shell effect plays a vital role in the stability of the nucleus not only at T=0, but also at finite temperature. This shell structure consider to be responsible for the formation of superheavy nuclei in the superheavy island. Thus, the microscopic model could be a better frame-work for such type of studies, where the shell structure of the nucleus is included automatically. In this aspect the Hartree or Hartree-Fock approach of non-relativistic mean field  or relativistic mean field (RMF)  formalisms could be some of the ideal theories.
The pioneering work of Vautherin and Brink , who has applied the Skyrme interaction in a self-consistent method for the calculation of ground state properties of finite nuclei opened a new dimension in the quantitative estimation of nuclear properties. Subsequently, the Hartree-Fock and time dependent Hartree-Fock formalisms  are also implemented to study the properties of fission. Most recently, the microscopic relativistic mean field approximation, which is another successful theory in nuclear physics is used for the study of nuclear fission . The RMF formalism is not only gaining importance for finite nuclei, but also quite useful for infinite nuclear matter systems. This theory successfully applied to study the gravitational wave strain and the tidal deformability in binary neutron stars merger . In the present paper, we have applied the recently developed FSUGarnet , and IOPB-I  models in the framework of temperature dependent effective field theory motivated relativistic mean field (E-RMF) formalism, which is the extended version of the standard nonlinear model by including all type of self and cross-couplings in the RMF Lagrangian. For comparison, the widely used NL3 force  is also applied in the calculations. Since, thermally fissile nuclei U, U and Pu undergo fission through the U, U and Pu respectively, as mentioned earlier, after absorbing a thermal neutron. Thus, we have studied the properties of hot U, U and Pb nuclei. Along with these nuclei, we have taken Pb as a representative case to examine our calculation for spherical nuclei.
The paper is organized as follows: In Section II, the finite temperature relativistic mean field theory is presented briefly. In this section, the equation of motion of the nucleon and meson fields are obtained from the relativistic mean field Lagrangian. The temperature dependent of the equations are adopted through the occupation number of protons and neutrons as it is developed in Refs. [3, 4]. The results are discussed in Section III and compared with various models, wherever necessary. The summary and concluding remarks are given in Section IV.
2 Theoretical Framework
2.1 Effective field theory motivated relativistic mean field formalism
From last five decades the relativistic mean field (RMF) formalism is one of the most successful and widely used theory for both finite nuclei and infinite nuclear matter systems including the study of neutron star (NS). It is nothing but the relativistic generalization of the non relativistic Hartree or Hartree-Fock Bogoliubov theory with the advantages that it takes into account the spin orbit interaction automatically and works better in high density region. In this theory, nucleons are considered to oscillate independently in a harmonic oscillator motion in the mean fields generated by the exchange of mesons and photons. The nucleons are interacted with each other through the exchange of isoscalar-scalar , isoscalar-vector and isovector-vector mesons. The , and photon fields are taken into account in the original RMF formalism, known as the linear model. In this approximation, the model predicts incompressibility of nuclear matter 550 MeV which is far away from the experimental value MeV . To rectify this limitation, Boguta and Bodmer included the self couplings of meson in the Lagrangian and hence, known as the non-linear model  which reduces the incompressibility of nuclear matter to a considerable range of MeV. It reproduces the nuclear bulk properties like binding energy BE, root mean square (rms) charge radius , neutron-skin thickness and quadrupole deformation parameter etc. remarkably well not only for the stable nuclei, but also for exotic nuclei which are far away from the stability valley. After the success of this model, a large number of force parameters have been proposed, which take into account various other mediating mesons and their self and cross couplings. These higher order couplings are quite important, because each and every coupling in the E-RMF Lagrangian has its own effect to explain various physical phenomena in different environments starting from very low to high density domains. As a result, parameter sets like FSUGarnet , IOPB-I , G1 , G2  and G3  have been evolved with time.
In this section, we briefly outline the effective field theory motivated relativistic mean field (E-RMF) theory . The model is used by fitting the coupling constants and mass of the meson to reproduce the known nuclear ground state properties of some spherical nuclei as well as the nuclear matter properties at saturation. In principle, the E-RMF Lagrangian has an infinite number of terms with all type of self and cross couplings. Thus, it is necessary to develop a truncation scheme to handle numerically for the calculations of finite and infinite nuclear matter properties. The meson fields included in the Lagrangian are smaller than the mass of nucleon. Their ratios are used as a truncation scheme as it is done in Refs. [33, 35, 36, 37]. This means , and are the expansion parameters. The constraint of naturalness is also introduced in the truncation scheme to avoid ambiguities in the expansion. In other words, the coupling constants written with a suitable dimensionless form should be . Imposing these conditions, one can then estimate the contributions coming from different terms of the Lagrangian by counting powers in the expansion up to a certain order of accuracy and the coupling constants should not be truncated arbitrarily. It is shown that the Lagrangian up to fourth order of dimension is a good approximation to predict finite nuclei and nuclear matter observables up to considerable satisfaction [33, 35, 36, 37]. Thus, in the present calculations, we have considered the contribution of the terms in the E-RMF Lagrangian up to order of expansion. The nucleon-meson E-RMF Lagrangian density with , , mesons and photon fields is given as [29, 30]:
Here , and are the mesonic fields having masses , and with coupling constants , and for , and mesons, respectively. is the photon field which is responsible for electromagnetic interaction with coupling strength . By using variational principle and applying mean field approximations, the equations of motion for the nucleon and boson fields are obtained. Redefining fields as , , and , the Dirac equation corresponds to the above Lagrangian density is
The mean field equations for , , and are given as
The baryon, scalar, isovector and proton densities used in the above equations are defined as
Where and have their usual meanings. We have taken summation over where stands for all nucleon. The factor , used in the density expressions is nothing but occupation probability which is described in the next sub-section. The effective mass of nucleon due to its motion in the mean field potential is given as and the vector potential is The energy densities for nucleonic and mesonic fields corresponding to the Lagrangian density are
To solve the set of coupled differential equations (5-9) we expand the Boson and Fermion fields in an axially deformed harmonic oscillator basis with as the initial deformation. The set of equations are solved self iteratively till the convergence is achieved. The center of mass correction is subtracted within the non-relativistic approximation . The calculation is extended to finite temperature T through the occupation number in the BCS pairing formalism. The quadrupole deformation parameter is estimated from the resulting quadrupole moments of the protons and neutrons as , (where fm ). The total energy at finite temperature T is given by [39, 40, 41],
Here, is the single particle energy, is the occupation probability and is the pairing energy obtained from the BCS formalism. The and are the probabilities of unoccupied and occupied states, respectively.
2.2 Pairing and temperature dependent E-RMF formalism
There are experimental evidences that even-even nuclei are more stable than even-odd or odd-odd isotopes. Thus, pairing correlation plays a distinct role in an open shell nuclei. The total binding energy of open shell nuclei deviates slightly from the experimental value when pairing correlation is not considered. To explain this effect, Aage Bohr, Ben Mottelson and Pines suggested BCS pairing in nuclei  just after the formulation of BCS theory for electrons in metals. The BCS pairing in nuclei is analogous to the pairing of electrons (Cooper pair) in super-conductors. It is used to explain energy gap in single particle spectrum. The detail formalism is given in Refs. [3, 4], but for completeness, we are briefly highlighting some essential part of the formalism. The BCS pairing state is defined as
where j and m are the quantum numbers of the state. In the mean field formalism, the violation of particle number is seen due to the pairing correlation, i.e., the appearance of terms like or , which are responsible for pairing correlations. Thus, we neglect such type of interaction at the RMF level and taking externally the pairing effect through the constant gap BCS pairing. The pairing interaction energy in terms of occupation probabilities and (where stands for nucleon) is written as [43, 44]:
with is the pairing force constant. The variational approach with respect to the occupation number gives the BCS equation :
The temperature introduced in the partial occupancies through the BCS approximation is given by,
The function represents the Fermi Dirac distribution for quasi particle energy . The chemical potential for protons (neutrons) is obtained from the constraints of particle number equations
The sum is taken over all the protons and neutrons states. The entropy is obtained by,
The total energy and the gap parameter are obtained by minimizing the free energy,
In constant pairing gap calculations, for a particular value of pairing gap and force constant , the pairing energy diverges, if it is extended to an infinite configuration space. In fact, in all realistic calculations with finite range forces, is not constant, but decreases with large angular momenta states above the Fermi surface. Therefore, a pairing window in all the equations are extended up-to the level as a function of the single particle energy. The factor 2 has been determined so as to reproduce the pairing correlation energy for neutrons in Sn using Gogny force [41, 43, 46].
3 Results and Discussions
The detail results of our calculations are presented in Table 2 and Figures . Here, we discuss the binding energy, nuclear radii, quadrupole and hexadecapole deformation parameters, specific heat, shell correction energy, inverse level density parameter, two neutron separation energy and asymmetry energy coefficient as a function of temperature T. First of all we will explain our motivation for the choice of parameter sets used and subsequently we will discuss the results of our calculations.
3.1 Parameter chosen
There are large number of parameter sets available in the literature [30, 34, 47]. All the forces are designed with an aim to explain certain nuclear phenomena either in normal or in extreme conditions. In a relativistic mean field Lagrangian, every coupling term has its own effect to explain some physical quantities. For example, the self-coupling terms in the meson takes care of the 3-body interaction which helps to explain the Coester band problem and the incompressibility coefficient of nuclear matter at saturation [24, 48, 49]. In the absence of these non-linear couplings, the earlier force parameters predict a large value of MeV [50, 51]. The non-linear term of the isoscalar vector meson plays a crucial role to soften the nuclear equation of state (EOS) . Adjusting this coupling constant , one can reproduce the experimental data of the sub-saturation density . The finite nuclear system is in the region of sub-saturation density and this coupling could be important to describe the phenomena of finite nuclei.
For a quite some time, the cross coupling of the isovector-vector meson and the isoscalar-vector meson is ignored in the calculations. Even the effective field theory motivated relativistic mean field (E-RMF) Lagrangian  does not include this term in its original formalism. For the first time, Todd-Rutel and Piekarewicz  realized the effect of this coupling in the correlation of neutron-skin thickness and the radius of neutron star. This coupling constant influences the neutron distribution radius without affecting much other properties like proton distribution radius or binding energy of finite nucleus. The RMF parameter set without coupling predicts a larger incompressibility coefficient than the non-relativistic Skyrme/Gogny interactions or empirical data. However, this value of agree with such predictions when the coupling present in the Lagrangian. Thus, the parameter can be used as a bridge between the non-relativistic and relativistic mean field models. Although, the contribution of this coupling is marginal for the calculation of bulk properties of finite nuclei, the inclusion of in the E-RMF formalism is important for its softening nature to nuclear equation of states. The inclusion of non-linear term of field and cross coupling of vector fields () reproduce experimental values of GMR and IVGDR well comparative to those of NL3, and hence, they are needed for reproducing a few nuclear collective modes . These two terms also soften both EOS of symmetric nuclear matter and symmetry energy.
In the present paper, the results are obtained from three different RMF sets, namely FSUGarnet , IOPB-I  and NL3 . The NL3 is the oldest among them and one of the most successful force for finite nuclei all over the mass table. It produces excellent results for binding energy, charge radius and quadrupole deformation parameter not only for stability nuclei, but also for nuclei away from the valley of stability. On the other hand the FSUGarnet is a recent parameter set . It is seen in Ref.  that this set reproduces the neutron-skin thickness with the recent data up to a satisfactory level along with other bulk properties. The IOPB-I is the latest in this series and reproduces the results with an excellent agreement with the data. It is to be noted that the FSUGarnet reproduces the neutron star mass in the lower limit, i.e., and the IOPB-I gives the upper limit of neutron star mass . These FSUGarnet and IOPB-I parameters have the additional non linear term of isoscalar vector meson and cross coupling of vector mesons over NL3 set. To our knowledge, for the first time the FSUGarnet and IOPB-I are used for the calculations of deform nuclei. Also, for the first time these two sets are applied to finite temperature calculations for nuclei. The values of the parameters and their nuclear matter properties are depicted in Table 1.
First of all, we want to compare our calculated results with the experimental data. The results of our calculations for binding energy per particle B/A, quadrupole deformation parameter and charge radius for Pb, U and Pu using FSUGarnet, IOPB-I and NL3 are tabulated in Table 2 at zero temperature. The experimental data are also given for comparison. From the table, it is clear that all the parameter sets reproduce the results remarkably well. A further inspection of the table indicates that some time, the binding energy predicted by IOPB-I overestimates the data. However, the deformation parameter is slightly smaller and the charge radius is slightly larger compared to the experimental measurements. In general, all the three observables are in an excellent agreement with the experimental observations and we can use the models for further predictions at different conditions, such as at finite temperature. Now we want to discuss some important nuclear properties at finite temperature with these three successful models in the following sub-sections.
3.2 Nuclear excitation energy and shell melting point
After verifying the validity of these force parameters by studying the nuclear properties at ground state (T = 0 MeV), we have extended the calculations to study further at finite temperature. As the temperature of a nucleus rises, the nucleons are excited to higher orbitals and the nucleus as a whole in an excited state. And hence, all its observables change with T. Before going to study other properties of a nucleus, first we discuss the variation of its binding energy with T. The binding energies for Pb, U and Pu are shown in Figure 1 with FSUGarnet, IOPB-I and NL3 sets. The binding energies in all the cases decrease gradually with the effect of temperature. It is found that at , all the three forces give almost same binding energy. This is clear from both Table 2 and Figure 1 for the cases, where the experimental data are measured precisely (). Also, the predicted results at coincide very much with the experimental data (see Figure 1 and Table 2). Further, with the increase of temperature, the BE corresponding to NL3 force underestimates the prediction of other two sets IOPB-I and FSUGarnet as shown in the figure.
The nuclear excitation energy is one of the key quantity in fission dynamics. The excitation energy very much depends on the state of the nucleus. It is defined as the nucleus excited how far from the ground state and can be measured from the relation , where E(T) is the binding energy of the nucleus at finite T and E(T=0) is the ground state binding energy. The variation of as a function of T is shown in Figure 2 for Pb, U and Pu with NL3, FSUGarnet and IOPB-I sets. One can see from the figure that the variation of excitation energy is almost quadratic in nature satisfying the relation . similar to the binding energy, the results of for FSUGarnet and IOPB-I coincide with each other, but the predicted by NL3 set overestimate these two as shown in Figure 2.
The excitation energy has a direct relation with the entropy S, i.e., the disorderness of the system. The expected relation of S with and the level density parameter from Fermi gas model is . However, this straight line relation of versus deviates at low excitation energy due to the shell structure of nucleus . The value of as a function of is shown in Figure 3 for the four considered nuclei. The intercept of the curve on the axis is a measure of shell correction energy to the nucleus. Thus the actual relation of with can be written as , where shell correction energy. Beyond these ”slope points” the versus curve increase in a straight line as shown in the figure (the slope point is marked by circle). Thus, one can interpret that beyond this particular excitation energy, the nucleus as a whole does not have a shell structure, and can be considered as the melting point of shell in the nucleus. The value of this point depends on the ground state shell structure of the nucleus. The, experimental evidences of washing out of the shell effects at and around 40 MeV excitation energy has also been pointed out in Ref . Shell correction obtained from the intercepts on the axis in Figure 3 are depicted in the figure for all four nuclei corresponding to parameters set considered here. For example, shell correction energies are , , and MeV for Pb, U and Pu respectively, corresponding to IOPB-I parameter set. The values for all three parameter sets are almost same with a little difference in NL3 model (see Figure 3).
A further analysis of the melting of shell, we calculate the nuclear shell correction energy for protons, neutrons and total nucleons of the nucleus. This, we have evaluated in the frame-work of the well known Strutinsky shell correction prescription . The relativistic single particle energies for protons and neutrons at finite T obtained by various sets (NL3, FUSGarnet and IOPB-I) are the inputs in the calculations and the results are depicted in Figure 4. As expected, the shell corrections (both protons and neutrons) for Pb, almost remains constant with temperature. Contrary to the behavior of Pb, the for U and Pu, initially increase with T for neutron up to the transition point and then suddenly decrease monotonously. On the other hand, we get an abrupt change of for proton at the transition point and remains a constant value as shown in Figure 4. This transition point, i.e., the shell melting point coincides with the results obtained from the curve (Figure 3).
In Figure 5, we plot the two-neutron separation energy with temperature T for Pb, U, U and Pu with FSUGarnet, IOPB-I and NL3 parameter sets. For Pb, there is no definite transition point in the 2n-separation energy. In case of U, all forces give the same transition point (i.e., Mev), whereas in U and Pu it is parameter dependent as shown in Figure 5. For example, in case of U we noticed the transition point for NL3 a bit later than IOPB-I and FSUGarnet but for Pu, the transition point is opposite in nature (see Figure 5). In addition, for Pb, the curves corresponding to FSUGarnet and IOPB-I sets overlap and distinct from NL3. The value decreases gradually for . But, for other three nuclei this behavior is different. There is a sudden fall at the transition temperature. Beyond these temperatures, the value decreases almost smoothly. Thus, It can be concluded from the graph that the probability of emission of neutrons grows as temperature increases. This probability become very high at and beyond transition points.
3.3 Single particle energy and shape transition
In Figure 6, we have shown a few single particle levels of neutrons for the nuclei Pb and U as a representing case with IOPB-I set. From the figure, it is clear that the single particle energy of various states arising from different orbitals merge to a single degenerate level with increase of temperature after a particular T for the U nucleus. We call this temperature as the shell melting or transition temperature, because this is the temperature at which the nucleus changes from deformed to spherical state and all the levels converged to a single degenerate one [59, 58]. The same value of critical temperature is obtained in case of single particle spectrum of protons for the nuclei, i.e., non-degenerate levels become the degenerate. The same behavior is obtained for the other remaining thermally fissile nuclei considered here. When we compare this temperature with the shell melting point (i.e. slope point of the vs curve), change in (Figure 4) and values (Figure 5), the merging point in matches perfectly with each other. We have increased the temperature further, and analyzed the single particle levels at higher T, but we have not noticed the re-appearance of non-degenerate states. In case of Pb, the single particle energy for proton and neutron do not change with temperature. This is because, there is no change in the shape of this nucleus as it is spherical throughout all the T. Although, the shell correction energy changes from negative to positive or vice versa, we have not found the disappearance of shell correction completely. This means, whatever be the temperature of the nucleus, the shell nature remains there, of course the nucleons are in the degenerate state. So, disappearance of shell effects implies the redistribution of shells at transition point i.e., from non-degenerate to degenerate. In other words, whatever be the temperature of the nucleus, there will be a finite value of shell correction energy (as shown in Figure 4) due to the random motion of nucleons. On inspecting the single-particle energy for the entire spectrum (not shown in the figure), one can find that low lying states raise slightly and high lying states decrease slightly. This is due to an increase in the effective mass and rms radius . We have repeated the calculations for other two parameter sets (NL3 and FSUGarnet) and find the same scenario.
3.4 Quadrupole and Hexadecapole deformations and shape transition
The quadrupole and hexadecapole deformation parameters for the nuclei U, U and Pu are shown in Figure 7. The upper panel is the and the lower panel is as a function of temperature T. Both the deformation parameters drastically decrease with T at . These results are qualitatively consistent with the previous studies for different nuclei [59, 60]. The almost zero value of at and beyond the critical temperature implies that the shape of nucleus changes form deformed to spherical. The non-smoothness on the surface of nucleus irrespective of its shape is defined by the hexadecapole deformation parameter . The same behavior for implies that on increasing temperature not only the shape of nucleus changes but also its surface becomes smooth. Hence nucleus becomes a perfectly degenerate sphere at temperature and beyond. We have checked that even on further increasing temperature the state of nucleus does not change again and remain spherical as mentioned earlier. While, in fission process, a nucleus undergoes scission point where it is highly deformed and hence, breaks into fragments. This observation concludes that the nucleus never undergoes fission only by temperature. It is necessary to disturb the nucleus physically for fission reaction bombarding thermal neutron. In other words, U, U and Pu have half-lives years, years and years, respectively. This means, these nuclei never undergo fission spontaneously whatever be the temperature. However, the fission reaction takes place whenever a zero energy (thermal) neutron hits on it externally.
3.5 Specific heat
For further study the phase transition at critical temperatures we have calculated specific heat for the nuclei considered here. The specific heat of a nucleus is:
The variation of specific heat with temperature is shown in Figure 8. The kinks in the curves for different nuclei correspond to the critical temperatures where shape transition takes place. This value differs with nucleus and in agreement with the obtained results shown in the previous graphs (Figures 3-7). But, it can be seen that for , there is no such kink which signifies that it remains spherical at all temperatures. The pattern of the curves is same as studied earlier for and . At low temperature FSUGarnet and IOPB-I results match and underestimates those of NL3 but at higher temperature i.e., beyond critical temperatures all the curves overlap with each others. The values of transition temperature are different for different parameter sets.
3.6 Root mean square radius
The root mean square radii for Pb, U, U and Pu are shown in Figure 9. The proton and neutron radii are presented in the upper panel whereas lower panel has the skin thickness for the nuclei. The rms radius, first increases slowly at lower temperature, and at higher temperature, it increases rapidly for . This behavior is consistent with that discussed in Refs. [59, 61]. For the remaining nuclei, the rms radius first decreases with temperature up to a point and beyond that point these values increase rapidly with temperature. This is because the deformed nucleus first undergoes phase transition to spherical shape and hence, radius decreases slightly and beyond the said point these increase rapidly. The numerical values of the transition temperatures are consistent with the shown values in the previous figures. It is also observed from the figure that neutron radius corresponding to IOPB-I and NL3 parameters matches with each other but overestimate that of FSUGarnet result. For proton radius, FSUGarnet and NL3 results are coincide and underestimate that of IOPB-I. The values of rms radius are minimum at transition temperatures. Behavior of skin thickness is also almost same as of nucleus radius. The kinks here correspond to the same transition temperatures.
There is a point to be discussed here that the neutron-skin thickness is an important quantity in the determination of EOS. Although, there is a large uncertainty in the determination of , even then some of the precise measurement are done . Recently, it is reported  using the Gravitational wave observation data GW170817 that the upper limit of should be 0.25 fm for . The calculated values of for NL3, FSUGarnet and IOPB-I are 0.28, 0.16 and 0.22 fm, respectively, which can be seen from Figure 9. The value of neutron-skin thickness obtained by IOPB-I is preferred over NL3 and FSUGarnet. As we know, NL3 predicts a larger value which gives a larger neutron star radius . Similarly, FSUGarnet predicts a smaller and expected a smaller neutron star radius.
3.7 Inverse level density parameter
Level density parameter is a key quantity in the study of nuclear fission . It is used to predict the probability of fission fragments, yield of fragments and ultimately angular distribution of fragments [4, 3]. The motivation behind choosing thermally fissile nuclei as discussed above is to study fission parameters at finite temperature which may be useful for theoretical and experimental fission study. Dependence of level density parameter on temperature and its sensitivity to parameters chosen are discussed below. It can be obtained using the excitation energy and entropy as follows:
The parameter obtained from equations (30) and (31) are equal, when it is independent of temperature . This is true for higher temperature i.e., beyond critical point. But, at low temperature, it is quite sensitive to T. The inverse level density parameter defined as (where A is the mass of the nucleus) is presented in Figure 10. The bold and dashed lines correspond to the K values obtained by using the above two equations (30) and (31) are represented by the symbols and . At low temperature, values of K shoot up and then it becomes smooth with the variation of temperature. The pattern of and are same and there is no appreciable change as temperature rises except the kinks which again correspond to critical points. The constant K shows the vanishing of shell structure of the nucleus at higher temperature (See Fig. 10). These excitation energies are consistent with those shown in Figure 3 wherein slope of versus curve representing level density parameter. It is clear from the figure that FSUGarnet and IOPB-I curves overlap with each other and overestimate the values obtained by NL3 model. This sensitivity of level density parameter on the choice of Lagrangian density will affect the fragment distributions in the fission process.
3.8 Asymmetry energy coefficient
The properties of hot nuclei play a vital role in both nuclear physics and astrophysics . These properties are the excitation energy, entropy, symmetry energy, and density distribution . Among these properties, symmetry energy and its dependence on density and temperature have a crucial role in understanding various phenomena in heavy ion collision, supernovae explosions, and neutron star [7, 8]. It is a measure of energy gain in converting isospin symmetric nuclear matter to asymmetric one. The temperature dependence of symmetry energy plays its role in changing the location of neutron drip line. It has key importance for the liquid-gas phase transition of asymmetric nuclear matter, the dynamical evolution of mechanism of massive star and the supernovae explosion .
Experimentally, nuclear symmetry energy is not a directly measurable quantity. It is extracted indirectly from the observables those are related to it [67, 68]. Theoretically, there are different definition for different systems. For infinite nuclear matter, symmetry energy is the expansion of binding energy per nucleon in terms of isospin asymmetry parameter, i.e., as :
where is the nucleon number density. The coefficient in the second term is the asymmetry energy coefficient of nuclear matter at density . The value of for nuclear matter at saturation density is about 30-34 MeV [69, 70, 71]. For finite nuclei, symmetry energy is defined as one of the contributing term due to asymmetry in the system in the Bethe-Weizsacker mass formula. The coefficient of symmetry energy is defined as 
where and are the volume and surface asymmetry energy coefficients. The is considered as the asymmetry energy coefficient of infinite nuclear matter at saturation density. Here, we have calculated asymmetry energy coefficient of the nucleus of mass number A at finite temperature by using the method [73, 74]:
where and are the neutron excess () of a pair of nuclei having same mass number A but different proton number Z. We have taken for calculating where, is the atomic number of the considered nucleus. The is the energy per particle obtained by subtracting Coulomb part, i.e., Coulomb energy due to exchange of photon in the interaction of nucleons is subtracted from the total energy of the nucleus (). For example, to study the asymmetry energy coefficient for U at temperature T using Eq. (34), we estimate the binding energy for U at finite temperature T without considering Coulomb contribution. Then the binding energy of Th is measured in the similar conditions, i.e. without Coulomb energy at temperature T. Here for Uranium and for Thorium with same mass number A=236 are chosen. Note that the value of need not be , but generally a pair of even-even nuclei are considered whose atomic number differer by 2. The temperature dependence coefficient for different isotopic chains had been studied by using various definition as mentioned above and with relativistic and non-relativistic Extended Thomas Fermi Model [61, 74, 75]. In Ref. , the effect of choosing different pairs of nuclei on coefficient is discussed.
The asymmetry energy coefficient for all four nuclei are shown in Figure 11. From the figure, one can not say that the asymmetry energy co-efficient follows a particular pattern. This value is highly force dependent and results of different nuclei have different trend with temperature. For example, in case of Pb, IOPB-I set consistently predicts smaller than those of NL3 and FSUGarnet. At low temperature, NL3 has the larger even than FSUGarnet, but for relatively high temperature of both NL3 and FSUGarnet coincide with each others. In case of U, the scenario is completely different. Here, FSUGarnet consistently predicts a larger than NL3 and IOPB-I. But, the values of NL3 and IOPB-I crosses each other at various places with increase of T. In case of Pu, although is smaller for IOPB-I, but magnitude-wise all the three results are almost similar to each other. All the three sets predict very different results with each other for U; FSUGarnet gives a nearly constant value throughout all the temperature, IOPB-I initially predicts constant behavior and suddenly decreases with T, but NL3 gives a consistently increasing value with T.
4 Summary and conclusions
In summary, for the first time we have applied the recently proposed FSUGarnet and IOPB-I parameter sets of E-RMF formalism to deform nuclei at finite temperature. The bulk properties of finite nuclei, such as binding energy, charge radius, quadrupole and hexadecapole deformation parameters are evaluated. In this context, we have chosen the U and Pu nuclei, because these compound nuclei are formed by absorbing a thermal neutron from their thermally fissile parents U and Pu, respectively. Our calculated results are compared with the prediction of the well known NL3 parameter set as well as with experimental data, wherever available. These properties for hot nuclei are of great importance in both nuclear fission and astrophysics. A detail analysis is also performed on excitation energy, shell structure including shell correction and melting of shell with temperature. The quadrupole and hexadecapole shape change with the effect of temperature are discussed elaborately. We found that and decrease with temperature and finally the nucleus attains a degenerate Fermi liquid. The nuclear asymmetry energy coefficient is a crucial quantity both for finite nucleus and nuclear matter. Here, we have studied the asymmetry energy coefficient with temperature and found that the coefficient has a diverse nature. It depends on the parameter sets and the nuclear systems.
The authors thank Bharat Kumar, P. Arumugam and B. K. Agrawal for fruitful discussions. AQ and KCN acknowledge Institute of Physics (IOP), Bhubaneswar for providing the necessary computer facility and hospitality. Abdul Quddus thanks to Department of Science and Technology, Govt. of India for the partial support in the form of INSPIRE fellowship. Partial financial support is also provided by the Department of Science and Technology, Govt. of India, Project No. EMR/2015/002517.
-  National Nucl. Data Center, www. nndc. bnl. gov.
-  O. Hahn and F. Strassmann, Naturwissenschaften 26, 755 (1938).
-  Bharat Kumar, M. T. Senthil Kannan, M. Balasubramaniam, B. K. Agrawal, and S. K. Patra, Phys. Rev. C 96, 034623 (2017).
-  M. T. Senthil Kannan, Bharat Kumar, M. Balasubramaniam, B. K. Agrawal, and S. K. Patra, Phys. Rev. C 95, 064613 (2017).
-  B. A. Brown, Phys. Rev. Lett. 85, 5296 (2000).
-  C. J. Horowitz and J. Piekarewicz, Phys. Rev. Lett. 86, 5647 (2001).
-  V. Baran, M. Colonna, V. Greco, and M. Di Toro, Phys. Rep. 410, 335 (2005).
-  J. M. Lattimer and M. Prakash, Phys. Rep. 442, 109 (2007).
-  E. Baron, J. Cooperstein, and S. Kahana, Phys. Rev. Lett. 55, 126 (1985).
-  P. Fong, Phys. Rev. C 3, 2025 (1971).
-  V. A. Rubchenya and S. G. Yavshits, Z. Physik A: At. Nucl. 329, 217 (1988).
-  J. P. Lestone, Phys. Rev. C 70, 021601 (2004).
-  P. Fong, Phys. Rev. 102, 434 (1956).
-  K. Manimaran and M. Balasubramanian, Phys. Rev. C 79, 024610 (2009).
-  J. Toke, et. al., Nucl. Phys. A 440, 327 (1985).
-  B. Borderie, et. al., Z Physik A: At. and Nucl. 299, 263 (1981).
-  V. S. Ramamurthy and S. S. Kapoor, Phys. Rev. Lett. 54, 178 (1985).
-  W J Swiatecki, Physica Scr. 24, 113 (1981).
-  H. Diehl and W. Greiner, Nucl. Phys. A 229, 29 (1974).
-  B. D. Wilkins, E. P. Steinberg, and R. R. Chasman, Phys. Rev. C 14, 1832 (1976).
-  H. C. Pauli and T. Ledergerver, Nucl. Phys. A 175, 545 (1971).
-  Herbert Diehl and Walter Greiner, Nucl. Phys. A. 229, 29 (1974).
-  M. Bender, P.-H. Heenen, and P.-G. Reinhard, Rev. Mod. Phys. 75, 121 (2003).
-  J. Boguta and A. R. Bodmer, Nucl. Phys. A 292, 413 (1977).
-  D. Vautherin and D. M. Brink, Phys. Lett. B 32, 149 (1970); Phys. Rev. C 5, 626 (1972).
-  M. K. Pal and A. P. Stamp, Nucl. Phys. A 99, 228 (1967).
-  S. K. Patra, R. K. Choudhury and L. Satpathy, J. Phys. G. 37, 085103 (2010).
-  Bharat Kumar, S. K. Biswal and S. K. Patra, Phys. Rev. C 95, 015801 (2017)
-  Wei-Chai Chen and J. Piekarewicz, Phys. Lett. B 748, 284 (2015).
-  Bharat Kumar, B. K. Agrawal and S. K. Patra, arXiv:1711.04940v2
-  G. A. Lalazissis, J. König and P. Ring, Phys. Rev. C 55, 540 (1997).
-  J. P. Blaizot, Phys. Rep. 64, 171 (1980).
-  R. J. Furnstahl, B. D. Serot and H. B. Tang, Nucl. Phys. A 598, 539 (1996); R. J. Furnstahl, B. D. Serot and H. B. Tang, Nucl. Phys. A 615, 441 (1997).
-  Bharat Kumar, S. K. Singh, B. K. Agrawal, and S. K. Patra, Nucl. Phys. A 966, 197 (2017).
-  H. Müller and B. D. Serot, Nucl. Phys. A 606, 508 (1996).
-  B. D. Serot and J. D. Walecka, Int. J. Mod. Phys. E 6, 515 (1997).
-  M. Del Estal, M. Centelles, X. Viñas and S. K. Patra, Phys. Rev. C 63, 024314 (2001).
-  J. W. Negele, Phys. Rev. C 1, 1260 (1970).
-  P. G. Blunden and M. J. Iqbal, Phys. Lett. B 196, 295 (1987).
-  P. G. Reinhard, Rep. Prog. Phys. 52, 439 (1989).
-  Y. K. Gambhir, P. Ring and A. Thimet, Ann. of Phys. 198, 132 (1990).
-  A. Bohr, B. R. Mottelson and D. Pines, Phys. Rev. 110, 4 (1958).
-  S. K. Patra, Phys. Rev. C 48, 1449 (1993).
-  M. A. Preston and R. K. Bhaduri, Structure of Nucleus, Addison-Wesley Publishing Company, Ch. 8, page 309 (1982).
-  D. Vautherin, Phys. Rev. C 7, 296 (1973).
-  J. Dechargé and D. Gogny, Phys. Rev. C 21, 1568 (1980).
-  M. Dutra, O. Lourenco, S. S. Avancini, B. V. Carlson, A. Delfino, D. P. Menezes, C. Providencia, S. Typel, and J. R. Stone, Phys. Rev. C 90, 055203 (2014).
-  J. I. Fujita and H. Miyazawa, Prog. Theor. Phys. 17, 360 (1957).
-  S. C. Pieper, V. R. Pandharipande, R. B. Wiringa, and J. Carlson, Phys. Rev. C 64, 014001 (2001).
-  B. D. Serot and J. D. Walecka, Adv. Nucl. Phys. 16, 1 (1986).
-  J. D. Walecka, Ann. Phys. 83, 491 (1974).
-  Y. Sugahara and H. Toki, Nucl. Phys. A 579, 557 (1994).
-  B. G. Todd-Rutel and J. Piekarewicz, Phys. Rev. Lett. 95, (2005) 122501; C. J. Horowitz and J. Piekarewicz, Phys. Rev. Lett. 86, (2001) 5647; Phys. Rev. C 64 (2001), 062802 (R).
-  I. Angeli, K. P. Morinova Atomic Data and Nuclear Data Table 99, 69 (2013).
-  V. S. Ramamurthy, S. S. Kapoor and S. K. Kataria, Phys. Rev. Lett. 25, 386 (1970).
-  A. Chaudhuri, et al., Phys. Rev. C 91, 044620 (2015).
-  V. M. Strutinsky, Nucl. Phys. A95, 420 (1967).
-  B. K. Agrawal, Tapas Sil, S. K. Samaddar, and J. N. De, Phys. Rev. C 64, 017304 (2001).
-  Y. K. Gambhir, J. P. Maharana, G. A. Lalazissis, C. P. Panos and P. Ring, Phys. Rev. C 62, 054610 (2000).
-  B. K. Agrawal, Tapas Sil, J. N. De, and S. K. Samaddar, Phys. Rev. C 62, 044307 (2000).
-  A. N. Antonov, D. N. Kadrev, and et al., Phys. Rev. C 95, 024314 (2017).
-  A. Trzcińska, J. Jastrzebski, P. Lubiński, F. J. Hartmann, R.Schmidt, T. von Egidy, and B. Klos, Phys. Rev. Lett. 87, 082501 (2001); J. Jastrzebski, A. Trzcińska, P. Lubiński, B.Klos, F. J. Hartmann, T. von Egidy, and S. Wycech, Int. J. Mod. Phys. E 13, 343 (2004).
-  F. J. Fattoyev, J. Piekarewicz and C. J. Horowitz, arXiv: 1711.06615v1; P. B. Abbott et. al., Phys. Rev. Lett. 119, 161101 (2017).
-  H. A. Bethe, Nuclear Phys. B. 9, 69 (1937).
-  B. K. Agrawal et al., Phys. Rev. C 58, 3004 (1998).
-  S. Sholom and V. M. Kolomietz, Rep. Prog. Phys. 68, 1 (2005).
-  D. V. Shetty and S. J. Yennello, Pramana 75, 259 (2010).
-  S. Kowalski et al., Phys. Rev. C 75, 014601 (2007).
-  J. N. De, S. K. Samaddar, and B. K. Agrawal, Phys. Lett. B 716, 361 (2012).
-  B. K. Agrawal, J. N. De, S. K. Samaddar, M. Centelles, and X. Viñas, Eur. Phys. J. A 50, 19 (2014).
-  P. G. Reinhard, M. Bender, W. Nazarewics, and T Vertse, Phys. Rev. C 73, 014309 (2006).
-  P. Danielewicz, Nucl. Phys. A 727, 233 (2003).
-  D. J. Dean, K. Langanke, and J. M. Sampaio, Phys. Rev. C 66, 045802 (2002).
-  J. N. De and S. K. Samaddar, Phys. Rev. C 85, 024310 (2012).
-  Z. W. Zhang, S. S. Bao, J. N. Hu, and H. Shen, Phys. Rev. C 90, 054302 (2014).