119526361
DECREASE OF THE SPIN-ORBIT INTERACTION IN DRIP-LINE NUCLEI, USING RELATIVISTIC MEAN FIELD MODELS
The spin-orbit potential and the energy splitting of spin-orbit partners in nuclei towards the neutron drip-line are found to show the decreasing behavior with the increase of neutron number, in both the spherical and deformed versions of the standard relativistic mean field model, the SRMF and DRMF, and its extended version for spherical case, the effective field theory motivated relativistic mean field model, the E-RMF. The calculations are presented for nuclei in different mass regions, which include the isotopes of F, Mg, Sb, Pb and Bi nuclei.
6024372
Superheavy nuclei in a relativistic effective Lagrangian model
Isotopic and isotonic chains of superheavy nuclei are analyzed to search for spherical double shell closures beyond Z= 82 and N= 126 within the new effective field theory model of Furnstahl, Serot, and Tang for the relativistic nuclear many-body problem. We take into account several indicators to identify the occurrence of possible shell closures, such as two-nucleon separation energies, two-nucleon shell gaps, average pairing gaps, and the shell correction energy. The effective Lagrangian model predicts N= 172 and Z= 120 and N= 258 and Z= 120 as spherical doubly magic superheavy nuclei, whereas N= 184 and Z= 114 show some magic character depending on the parameter set. The magicity of a particular neutron (proton) number in the analyzed mass region is found to depend on the number of protons (neutrons) present in the nucleus.
119377917
Nuclear reaction studies of unstable nuclei using relativistic mean field formalisms in conjunction with the Glauber model
We study nuclear reaction cross sections for stable and unstable projectiles and targets within Glauber model, using densities obtained from various relativistic mean-field formalisms. The calculated cross sections are compared with the experimental data in some specific cases. We also evaluate the differential scattering cross sections at several incident energies and observe that the results found from various densities are similar at smaller scattering angles, whereas a systematic deviation is noticed at large angles. In general, these results agree fairly well with the experimental data.
119341992
Phase transition and properties of a compact star
We investigate the phase transition to a deconfined phase and the consequences in the formation of neutron stars. We use the recently proposed effective-field-theory-motivated relativistic mean-field theory for the hadrons and the MIT bag model and color-flavor locked (CFL) phase for the quark matter to get the appropriate equation of state. The properties of the stars are then calculated. The differences between unpaired and CFL quark matter are discussed.
118427586
Role of isospin physics in supernova matter and neutron stars
We investigate the liquid-gas phase transition of hot protoneutron stars shortly after their birth following supernova explosion and the composition and structure of hyperon-rich (proto)neutron stars within a relativistic mean-field model where the nuclear symmetry energy was constrained from the measured neutron skin thickness of finite nuclei. Light clusters are abundantly formed with increasing temperature well inside the neutrino-sphere for a uniform supernova matter. Liquid-gas phase transition is found to suppress the cluster yield within the coexistence phase as well as decrease considerably the neutron-proton asymmetry over a wide density range. We find symmetry energy has a modest effect on the boundaries and the critical temperature for the liquid-gas phase transition, and the composition depends more sensitively on the number of trapped neutrinos and temperature of the protoneutron star. The influence of hyperons in the dense interior of stars makes the overall equation of state soft. However, neutrino trapping distinctly delays the appearance of hyperons because of an abundance of electrons. We also find that a softer symmetry energy further makes the onset of hyperon less favorable. The resulting structures of the (proto)neutron stars with hyperons and with liquid-gas phase transition are discussed.
121406020
Exotic clustering in heavy and superheavy nuclei within the relativistic and non-relativistic mean field formalisms
The clustering phenomenon in heavy and superheavy nuclei is studied within the relativistic mean field (RMF) approach using axially deformed basis and the non-relativistic Skyrme?Hartree?Fock (SHF) formalism. The calculated ground and intrinsic excited state properties, and the total matter densities as well as the neutron?proton asymmetry distributions are analysed to look for the cluster configurations and/or exotic clusters in the known cluster emitting 222Ra, 232U, 236Pu and 242Cm nuclei, and the superheavy nuclei with Z = 114, N = 172?184. Both the theories predict N ? Z, ?-like matter or clustering in the ground states, and both N ? Z matter and N ? Z clustering in the excited intrinsic states of radioactive actinides, though this result is more apparent and universal for the RMF approach. For superheavy nuclei, the detailed analysis shows a non-clustering, 'bubble'-like structure for Z = 114, N = 184 nucleus in the RMF method and Z = 114, N = 176 or 180 nucleus in the SHF method, as the signatures of doubly closed shell nuclei. Our earlier similar calculations for Z = 120 nuclei predicted the same for Z = 120, N = 172 nucleus in the RMF model. Also, in contrast to radioactive actinides, in superheavy nuclei the two fragments, N ? Z cluster configurations at the centre of ground superdeformed states in the RMF approach, and the same for at least some of the excited superdeformed states in the SHF method, are some of the interesting results obtained. Thus, new possibilities of exotic clusters at the centre of superheavy nuclei are indicated as ground or excited intrinsic superdeformed state configurations, more so as ground superdeformed states in the RMF theory. The N/Z ratios of the clusters are also calculated on the basis of the (average value of) colour code of the contours, which give a reasonable correspondence with the experimental data on cluster decay of radioactive nuclei.
118316994
Irregularly Shaped Satellites-Phobos & Deimos- moons of Mars, and their evolutionary history
Phobos, a moon of Mars, is below the Clarke synchronous orbit and due to tidal interaction is losing altitude. With this altitude loss it is doomed to the fate of total destruction by direct collision with Mars. On the other hand Deimos, the second moon of Mars is in extra-synchronous orbit and almost stay put in the present orbit. The reported altitude loss of Phobos is two meter per century by wikipedia and sixty ft per century according to ozgate url . The reported time in which the destruction will take place is fiftyMy and fortyMy respectively. The authors had proposed a planetary-satellite dynamics based on detailed study of Earth-Moon. Based on this planetary satellite dynamics, two meter/century approach velocity leads to the age of Phobos to be twenty three Gyrs which is physically untenable since our Solar System age is four and a half Gyrs. Hence the present altitude loss is assumed to be twenty meter per century. This leads to the age of Phobos to be two decimal three Gyrs and age of Deimos to be two decimal two six Gyrs which is an acceptable result and from this analysis it is predicted that the travel time from the present orbital radius of nine thousand three hundred and eighty km to the Martian surface at three thousand, three hundred and ninety seven km is ten decimal and four Myrs. Hence doomsday of Phobos is at ten decimal and fourMyrs from now. Mars Express studies have confirmed that Phobos is indeed trapped in a death spiral.
122881907
NUCLEON–NUCLEUS OPTICAL POTENTIAL FROM HARD- AND SOFT-CORE INTERNUCLEON POTENTIALS
We have compared the binding energy of nuclear matter and the nucleon–nucleus optical potential, calculated in Brueckner theory starting from both the soft-core Urbana V-14 and the hard-core Hamada–Johnston internucleon potentials. Our results show that the real central part of the optical potential calculated from V-14 is about 10 MeV deeper than from the hard-core potential in the energy region 1–200 MeV. This greater depth mainly comes from the internucleon S- and D-states. In these states, the V-14 and Hamada–Johnston potentials give different phase shifts, the V-14 being in better agreement with experimental data. This difference is further enhanced by the Pauli principle in the calculation of the optical potential. Our analysis of proton–40Ca differential cross-section and polarization data, in the energy region 30–200 MeV, shows that the optical potential calculated using V-14 is in better agreement with the data as compared with the Hamada–Johnston potential.