A systematic study was conducted on the theoretical estimation of the nuclear cross sections of charged particle induced reactions on rare earth nuclei.The production cross sections of the ^(150,149,148,146,144,143,14...A systematic study was conducted on the theoretical estimation of the nuclear cross sections of charged particle induced reactions on rare earth nuclei.The production cross sections of the ^(150,149,148,146,144,143,141)Pm and ^(149,147)Nd nuclei were calculated theoretically via proton induced reactions on neodymium using TALYS(version 1.96)code in the default mode,with different combinations of nuclear models as well as adjusted nuclear model parameters from the reaction threshold up to a proton energy of 65 MeV.The theoretically computed results were compared with the experimental results taken from the EXFOR database and literature reported by various research groups.Moreover,the effects of various level density models,preequilibrium models,optical model potentials,and gamma strength functions on the cross section calculation were considered.This theoretical analysis will help elucidate the theory of nuclear reaction models and improve the evaluated nuclear data libraries.展开更多
A class of relativistic astrophysical compact objects is analyzed in the modified Finch-Skea geometry described by the MIT bag model equation of state of interior matter,p=1/3(ρ-4B),where B is known as the bag consta...A class of relativistic astrophysical compact objects is analyzed in the modified Finch-Skea geometry described by the MIT bag model equation of state of interior matter,p=1/3(ρ-4B),where B is known as the bag constant.B plays an important role in determining the physical features and structure of strange stars.We consider the finite mass of the strange quark(m_(s)≠0) and study its effects on the stability of quark matter inside a star.We note that the inclusion of strange quark mass affects the gross properties of the stellar configuration,such as maximum mass,surface red-shift,and the radius of strange quark stars.To apply our model physically,we consider three compact objects,namely,(ⅰ) VELA X-1,(ⅱ) 4U 1820-30,and(ⅲ) PSR J 1903+327,which are thought to be strange stars.The range of B is restricted from 57.55 to Bstable(MeV/fm3),for which strange matter might be stable relative to iron(^(56)Fe).However,we also observe that metastable and unstable strange matter depend on B and ms.All energy conditions hold well in this approach.Stability in terms of the Lagrangian perturbation of radial pressure is studied in this paper.展开更多
In this article,a new class of solutions of Einstein-Maxwell field equations of relativistic strange quark stars obtained in dimensions D≥4,is shown.We assume that the geometry of space-time is pseudo-spheroid,embedd...In this article,a new class of solutions of Einstein-Maxwell field equations of relativistic strange quark stars obtained in dimensions D≥4,is shown.We assume that the geometry of space-time is pseudo-spheroid,embedded in Euclidean space of(D-1)dimensions.The MIT bag model equation of state(henceforth EoS)is employed to study the relevant properties of strange quark stars.For the causal and non-negative nature of the square of the radial sound velocity(vr2),we observe that some restrictions exist on the reduced radius(b/R),where R is a parameter related to the curvature of the space-time,and b is the radius of the star.The spheroidal parameter A used here defines the metric potential of the grrcomponent,which is pseudo-spheroidal in nature.We note that the pressure anisotropy and charge have some effects onλ.The maximum mass for a given surface density(ρs)or bag constant(B)assumes a maximum value in dimension D=5and decreases for other values of D.The generalized Buchdahl limit for a higher dimensional charged star is also obeyed in this model.We observe that in this model,we can predict the mass of a strange quark star using a suitable value of the electric charge(Q)and bag constant(B).Energy and stability conditions are also satisfied in this model.Stability is also studied considering the dependence of the Lagrangian perturbation of radial pressure(Δpr)on the frequency of normal modes of oscillations.The tidal Love number and tidal de-formability are also evaluated.展开更多
基金ICFAI University Tripura for all their help and support in carrying out the research
文摘A systematic study was conducted on the theoretical estimation of the nuclear cross sections of charged particle induced reactions on rare earth nuclei.The production cross sections of the ^(150,149,148,146,144,143,141)Pm and ^(149,147)Nd nuclei were calculated theoretically via proton induced reactions on neodymium using TALYS(version 1.96)code in the default mode,with different combinations of nuclear models as well as adjusted nuclear model parameters from the reaction threshold up to a proton energy of 65 MeV.The theoretically computed results were compared with the experimental results taken from the EXFOR database and literature reported by various research groups.Moreover,the effects of various level density models,preequilibrium models,optical model potentials,and gamma strength functions on the cross section calculation were considered.This theoretical analysis will help elucidate the theory of nuclear reaction models and improve the evaluated nuclear data libraries.
基金BD and KBG thank the CSIR for providing the fellowship vide No 09/1219(0005)/2019-EMR-I and 09/1219(0004)/2019-EMR-I,respectively.
文摘A class of relativistic astrophysical compact objects is analyzed in the modified Finch-Skea geometry described by the MIT bag model equation of state of interior matter,p=1/3(ρ-4B),where B is known as the bag constant.B plays an important role in determining the physical features and structure of strange stars.We consider the finite mass of the strange quark(m_(s)≠0) and study its effects on the stability of quark matter inside a star.We note that the inclusion of strange quark mass affects the gross properties of the stellar configuration,such as maximum mass,surface red-shift,and the radius of strange quark stars.To apply our model physically,we consider three compact objects,namely,(ⅰ) VELA X-1,(ⅱ) 4U 1820-30,and(ⅲ) PSR J 1903+327,which are thought to be strange stars.The range of B is restricted from 57.55 to Bstable(MeV/fm3),for which strange matter might be stable relative to iron(^(56)Fe).However,we also observe that metastable and unstable strange matter depend on B and ms.All energy conditions hold well in this approach.Stability in terms of the Lagrangian perturbation of radial pressure is studied in this paper.
基金CSIR for providing fellowships vide no:09/1219(0004)/2019 EMR-I,CSIR for providing fellowships vide no:09/1219(0005)/2019 EMR-I。
文摘In this article,a new class of solutions of Einstein-Maxwell field equations of relativistic strange quark stars obtained in dimensions D≥4,is shown.We assume that the geometry of space-time is pseudo-spheroid,embedded in Euclidean space of(D-1)dimensions.The MIT bag model equation of state(henceforth EoS)is employed to study the relevant properties of strange quark stars.For the causal and non-negative nature of the square of the radial sound velocity(vr2),we observe that some restrictions exist on the reduced radius(b/R),where R is a parameter related to the curvature of the space-time,and b is the radius of the star.The spheroidal parameter A used here defines the metric potential of the grrcomponent,which is pseudo-spheroidal in nature.We note that the pressure anisotropy and charge have some effects onλ.The maximum mass for a given surface density(ρs)or bag constant(B)assumes a maximum value in dimension D=5and decreases for other values of D.The generalized Buchdahl limit for a higher dimensional charged star is also obeyed in this model.We observe that in this model,we can predict the mass of a strange quark star using a suitable value of the electric charge(Q)and bag constant(B).Energy and stability conditions are also satisfied in this model.Stability is also studied considering the dependence of the Lagrangian perturbation of radial pressure(Δpr)on the frequency of normal modes of oscillations.The tidal Love number and tidal de-formability are also evaluated.
