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nucl-th2025
Constraints on maximum neutron star mass from proto-neutron star evolution
Deepak Kumar, Tuhin Malik, Hiranmaya Mishra +1
A proto-neutron star (PNS) gets formed after a successful supernova when the stellar remnant decouples from the ejecta. In this study, we explore a relativistic framework for the f…
hep-ph2025
Axion effects on the non-radial oscillations of neutron stars
Deepak Kumar, Hiranmaya Mishra
The effects of axions on quark matter equation of state (EOS) is studied within the three flavor Nambu--Jona-Lasinio model and its effects on on the non-radial oscillations of neut…
nucl-th2025
Constraining the neutron star equation of state by including the isoscalar-vector and isovector-vector coupling using the Bayesian analysis
Deepak Kumar, Pradip Kumar Sahu
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 lev…