Nuclear symmetry energy from effective interaction and masses of isospin asymmetric nuclei

Mukhopadhyay, Tapan; Basu, Debabrata

doi:10.1016/j.nuclphysa.2007.04.006

Cited by 20 publications

(11 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The theoretical estimate for value of the NSE at saturation density E sym (ρ 0 )=30.71±0. 26 MeV obtained from the present calculations (DDM3Y) is reasonably close to the value of S v =30.048 ±0.004 MeV extracted [43] from the measured atomic mass excesses of 2228 nuclei. The value of NSE at ρ 0 remains mostly the same which is 30.03±0.26 MeV if one uses the mathematical definition of…”

Section: B Nuclear Symmetry Energy and Its Slope Incompressibility An...supporting

confidence: 90%

Gravitational waves from isolated neutron stars: Mass dependence of r -mode instability

et al. 2018

View full text Add to dashboard Cite

In this work we study the r-mode instability windows and the gravitational wave signatures of neutron stars in the slow rotation approximation using the equation of state obtained from the density dependent M3Y effective interaction. We consider the neutron star matter to be βequilibrated neutron-proton-electron matter at the core with a rigid crust. The fiducial gravitational and viscous timescales, the critical frequencies and the time evolutions of the frequencies and the rates of frequency change are calculated for a range of neutron star masses. We show that the young and hot rotating neutron stars lie in the r-mode instability region. We also emphasize that if the dominant dissipative mechanism of the r-mode is the shear viscosity along the boundary layer of the crust-core interface, then the neutron stars with low L value lie in the r-mode instability region and hence emit gravitational radiation.

show abstract

Section: B Nuclear Symmetry Energy and Its Slope Incompressibility An...supporting

confidence: 90%

Gravitational waves from isolated neutron stars: Mass dependence of r -mode instability

et al. 2018

View full text Add to dashboard Cite

show abstract

“…The volume symmetry energy coefficient S v extracted from nuclear masses provides a constraint on the NSE at nuclear density E sym (ρ 0 ). The value of S v =30.048 ±0.004 MeV extracted [44] from the measured atomic mass excesses of 2228 nuclei is reasonably close to the theoretical estimate of the value of NSE at saturation density E sym (ρ 0 )=30.71±0.26 MeV obtained from the present calculations using DDM3Y interaction. If one uses the alternative definition of E sym (ρ) = 1 2…”

Section: B Incompressibility Isobaric Incompressibility Symmetry Esupporting

confidence: 88%

From nuclear reactions to compact stars: A unified approach

Basu

Chowdhury²,

Mishra

2014

Eur. Phys. J. Plus

View full text Add to dashboard Cite

An equation of state (EoS) for symmetric nuclear matter is constructed using the density dependent M3Y effective interaction and extended for isospin asymmetric nuclear matter. Theoretically obtained values of symmetric nuclear matter incompressibility, isobaric incompressibility, symmetry energy and its slope agree well with experimentally extracted values. Folded microscopic potentials using this effective interaction, whose density dependence is determined from nuclear matter calculations, provide excellent descriptions for proton, alpha and cluster radioactivities, elastic and inelastic scattering. The nuclear deformation parameters extracted from inelastic scattering of protons agree well with other available results. The high density behavior of symmetric and asymmetric nuclear matter satisfies the constraints from the observed flow data of heavy-ion collisions. The neutron star properties studied using β-equilibrated neutron star matter obtained from this effective interaction for pure hadronic model agree with the recent observations of the massive compact stars such as PSR J1614-2230, but if a phase transition to quark matter is considered such agreement is no longer possible.

show abstract

“…The volume symmetry energy coefficient S v extracted from nuclear masses provides a constraint on the NSE at nuclear density E sym (ρ 0 ). The value of S v =30.048 ±0.004 MeV extracted [26] from the measured atomic mass excesses of 2228 nuclei is reasonably close to the theoretical estimate of the value of NSE at saturation density E sym (ρ 0 )=30.71±0. 26 MeV obtained from the present calculations using DDM3Y interaction.…”

Section: Incompressibility Isobaric Incompressibility Symmetry Energy...supporting

confidence: 83%

Effective interaction: From nuclear reactions to neutron stars

Basu

2013

Preprint

View full text Add to dashboard Cite

An equation of state (EoS) for symmetric nuclear matter is constructed using the density dependent M3Y effective interaction and extended for isospin asymmetric nuclear matter. Theoretically obtained values of symmetric nuclear matter incompressibility, isobaric incompressibility, symmetry energy and its slope agree well with experimentally extracted values. Folded microscopic potentials using this effective interaction, whose density dependence is determined from nuclear matter calculations, provide excellent descriptions for proton, alpha and cluster radioactivities, elastic and inelastic scattering. The nuclear deformation parameters extracted from inelastic scattering of protons agree well with other available results. The high density behavior of symmetric and asymmetric nuclear matter satisfies the constraints from the observed flow data of heavy-ion collisions. The neutron star properties studied using β-equilibrated neutron star matter obtained from this effective interaction reconcile with the recent observations of the massive compact stars.

show abstract

Nuclear symmetry energy from effective interaction and masses of isospin asymmetric nuclei

Cited by 20 publications

References 36 publications

Gravitational waves from isolated neutron stars: Mass dependence of r -mode instability

Gravitational waves from isolated neutron stars: Mass dependence of r -mode instability

From nuclear reactions to compact stars: A unified approach

Effective interaction: From nuclear reactions to neutron stars

Contact Info

Product

Resources

About