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).

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.

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.

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 properties of finite nuclei, bulk nuclear matter, and neutron stars are studied using the relativistic mean field model which includes nonlinear couplings between isoscalar and isovector mesons. The quartic interaction sigma 282 due to isoscalar and isovector scalar, sigma and 8 mesons, is also taken into account in addition to vector meson mixing w2p2. Several HPNL sets (named from Himachal Pradesh University Nuclear Laboratory) are generated to assess the influence of isoscalar and isovector scalar meson mixed interactions sigma 282 on the density dependence of symmetry energy and neutron star properties. These parametrizations correspond to different values of coupling constant, A sigma 8 of sigma -8 meson mixing and are obtained by fitting the available experimental data of ground state properties (binding energies and charge radii) for finite nuclei, infinite nuclear matter, and observed maximum mass of PSR J0740+6620 by following the X2 minimization procedure. Furthermore, the sigma-8 mixing is found to have a large influence on the radius and tidal deformability of a canonical neutron star. These new relativistic interactions are found to be simultaneously compatible with the constraints on the equation of state of symmetric nuclear and pure neutron matter from particle flow data in heavy ion collisions, the neutron skin thickness of 208Pb from PREX-II results, the mass-radius relations measured from NICER, and the limits of dimensionless tidal deformability of a canonical neutron star from binary neutron star merger GW170817 and GW190814 events.

In the present work, we investigate the bulk properties of nuclear matter and neutron stars with the newly proposed relativistic parametrizations HPUA, HPUB and HPUC which provides an opportunity to readjust the coupling parameters keeping in view the properties of finite nuclei, nuclear matter and astrophysical constraints. The HPUA, HPUB and HPUC are proposed by fitting both PREX-II + CREX results simultaneously, PREX-II and CREX results for neutron skin thickness of 208Pb and 48Ca respectively to assess their implications. The relativistic parameterizations have been generated by including non linear self-interactions of σ and ω- mesons and mixed interactions of ω, and ρ-meson up to the quartic order. The new equations of state (EoSs) composed of nucleons and leptons in β - equilibrium are constructed with the newly proposed parameter sets. The maximum mass of the neutron star by employing the EoSs computed with the HPU's parameter sets lies in the range 2.02±0.03 M⊙ - 2.04±0.03 M⊙ and the radius of canonical neutron star (R1.4) comes out to be equal to 12.89±0.08 Km - 13.27±0.30 Km (including BPS crust). The value of dimensionless tidal deformability, for canonical mass, is 590.83±22.58 - 631.52±78.13 which satisfies the constraints of waveform models analysis of GW170817. A covariance analysis is also performed to calculate the statistical uncertainties in the model parameters and nuclear matter observables along with their correlations.

We investigate the implications of parity-violating electron scattering experiment on neutron skin thickness of $^{48}$Ca (CREX) and $^{208}$Pb (PREX-II) data on the bulk properties of finite nuclei, nuclear matter, and neutron stars. The neutron skin thickness from the CREX and PREX-II data is employed to constrain the parameters of relativistic mean field models which includes different non-linear, self and cross-couplings among isoscalar-scalar $\sigma$, isoscalar-vector $\omega$, isovector-scalar $\delta$ and isovector-vector $\rho$ meson fields up to the quartic order. Three parametrizations of RMF model are proposed by fitting CREX, PREX-II and both CREX as well as PREX-II data to assess their implications. A covariance analysis is performed to assess the theoretical uncertainties of model parameters and nuclear matter observables along with correlations among them. The RMF model parametrization obtained with the CREX data acquires much smaller value of symmetry energy (J= 28.97$\pm$ 0.99 MeV), its slope parameter (L= 30.61$\pm 6.74$ MeV) in comparison to those obtained with PREX-II data. The neutron star properties are studied by employing the equations of state (EoSs) composed of nucleons and leptons in $\beta$ equilibrium.

C-reactive protein (CRP) is an annular (ring-shaped), pentamericprotein found in the blood plasma, the levels of which rise in response to inflammation (i.e., C-reactive protein is an acute-phase protein of hepatic origin that increases following interleukin-6 secretion from macrophages and T cells). Present study is aimed to find out the effects of practice of Shatkarma (Vaman, Jalneti&Kapalbhati) and Panchakarma (Vaman&Nasya) on C reactive protein in human subjects. The result revealed that post-experiment C reactive protein was lower than that of preexperiment.

A comparative study of different types of sense amplifiers [1] using 0.18um technology is presented. The sense amplifiers under considerations are used in SRAM and DRAM cells.The sensing delay of different types of sense amplifiers are evaluated with respect to variation of bitline capacitance. Comparative results are also provided for the variation in delay with respect to power supply. Extensive results based on 0.18um CMOS technology using CADENCE Spectre simulation tools are presented for different architectures of sense amplifiers. From these results it has been proven that if the output of sense amplifier is isolated from the bitline parasitic capacitance then the sensing delay of sense amplifier reduces.

Education is perceived to be universal phenomenon. It is adequately organized and regulated through formal institutions like colleges and schools. There are different factors, which determine the quality of education and its contribution to nation. The quality, competence, character and effectiveness of teachers are undoubtedly very significant. In developing society, a teacher has assumed a greater responsibility to bring out good citizens who could carry out the profession in a dignified and productive manner. To support the work of the organization teachers must have not only technical management skill but also skill in managing emotions, their as well as those of other individuals in the organization. Emotional competent teacher exhibits a high regard for colleagues and subordinates, an understanding of basic motivations as well as basic justice, as willingness to correct faculty situations, and a willingness to take positive, quick, and aggressive action when indicated. In this context the investigators conducted a study of Emotional Competence of 200 senior secondary school teachers. The major objectives of the study were to compare the Emotional Competence of male and female, rural and urban teachers. The Emotional Competence Scale (ECS) by H.C. Sharma and R. Bharadwaj was used to assess the effectiveness of teachers. Mean, S.D. and't’ test were used to analyze the data. The results indicated that no significant difference was found in Emotional Competence of teachers on the basis of gender whereas a significant difference has been found in Emotional Competence of teachers on the basis of their age and type of school.