REVIEW 1 cited by
Constraining the neutron star equation of state by including the isoscalar-vector and isovector-vector coupling using the Bayesian analysis
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
We constrain the nuclear matter equation of state within the relativistic mean field model by including the isoscalar-vector and isovector-vector coupling term at a fundamental level using the Bayesian analysis. We used the nuclear saturation properties and recent astrophysical observations to constrain the dense matter equation of state. We obtained about 20000 sets of equations of states out of sampling about 60 millions sets of equations of states. All 20000 equations of states satisfy nuclear matter saturation properties at saturation densities and produces high mass neutron stars. In our findings, we find that the non-zero value of isoscalar-vector and isovector-vector coupling parameter and negative value of sigma meson self-coupling stiffen the equation of state. Our sets of equations of state produces neutron stars of mass larger than 2.5 M$_{\odot}$ to include the recent gravitational waves observation GW190419.
Forward citations
Cited by 1 Pith paper
-
Constraints on maximum neutron star mass from proto-neutron star evolution
Hyperonic neutron stars are inferred to cap at roughly 2.15 to 2.2 solar masses, while stars above 2.2 solar masses should have purely nucleonic cores.
Discussion (0). Sign in to comment.