The massradius relationship of massive compact stars
Abstract
The properties of pure hadronic and hybrid compact stars are reviewed using nuclear equation of state (EoS) for βequilibrated neutron star (NS) matter obtained using a densitydependent M3Y (DDM3Y) effective nucleonnucleon interaction. Depending on the model, the energy density of quark matter can be lower than that of this nuclear EoS at higher densities, implying the possibility of transition to quark matter inside the core and the transition density depends on the particular quark matter model used. The recent observations of the binary millisecond pulsar J1614–2230 by P.B. Demorest et al. [1] and PSR J0348+0432 by J. Antoniadis et al. [2] suggest that the masses lie within 1.97 ± 0.04 M{sub ⊙} and 2.01 ± 0.04 M{sub ⊙}, respectively, where M{sub ⊙} is the solar mass. In conformity with recent observations, a pure nucleonic EoS determines that the maximum mass of NS rotating with frequency ν∼ 667 Hz below rmode instability is ∼ 1.95 M{sub ⊙} with radius ∼ 10 km. Compact stars with quark cores rotating with same frequency have the maximum mass of ∼ 1.72 M{sub ⊙} turns out to be lower than the observed masses.
 Authors:
 Department of Physics, Govt. Degree College Kamalpur, Tripura University, Tripura799285 (India)
 Publication Date:
 OSTI Identifier:
 22390990
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: AIP Conference Proceedings; Journal Volume: 1645; Journal Issue: 1; Conference: Carpathian Summer School of Physics 2014, Sinaia (Romania), 1326 Jul 2014; Other Information: (c) 2015 AIP Publishing LLC; Country of input: International Atomic Energy Agency (IAEA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ENERGY DENSITY; EQUATIONS OF STATE; HADRONS; INSTABILITY; M CODES; MASS; NEUTRON STARS; NUCLEONNUCLEON INTERACTIONS; PULSARS; QUARK MATTER; QUARKS
Citation Formats
Chowdhury, Partha Roy, Email: royc.partha@gmail.com. The massradius relationship of massive compact stars. United States: N. p., 2015.
Web. doi:10.1063/1.4909593.
Chowdhury, Partha Roy, Email: royc.partha@gmail.com. The massradius relationship of massive compact stars. United States. doi:10.1063/1.4909593.
Chowdhury, Partha Roy, Email: royc.partha@gmail.com. 2015.
"The massradius relationship of massive compact stars". United States.
doi:10.1063/1.4909593.
@article{osti_22390990,
title = {The massradius relationship of massive compact stars},
author = {Chowdhury, Partha Roy, Email: royc.partha@gmail.com},
abstractNote = {The properties of pure hadronic and hybrid compact stars are reviewed using nuclear equation of state (EoS) for βequilibrated neutron star (NS) matter obtained using a densitydependent M3Y (DDM3Y) effective nucleonnucleon interaction. Depending on the model, the energy density of quark matter can be lower than that of this nuclear EoS at higher densities, implying the possibility of transition to quark matter inside the core and the transition density depends on the particular quark matter model used. The recent observations of the binary millisecond pulsar J1614–2230 by P.B. Demorest et al. [1] and PSR J0348+0432 by J. Antoniadis et al. [2] suggest that the masses lie within 1.97 ± 0.04 M{sub ⊙} and 2.01 ± 0.04 M{sub ⊙}, respectively, where M{sub ⊙} is the solar mass. In conformity with recent observations, a pure nucleonic EoS determines that the maximum mass of NS rotating with frequency ν∼ 667 Hz below rmode instability is ∼ 1.95 M{sub ⊙} with radius ∼ 10 km. Compact stars with quark cores rotating with same frequency have the maximum mass of ∼ 1.72 M{sub ⊙} turns out to be lower than the observed masses.},
doi = {10.1063/1.4909593},
journal = {AIP Conference Proceedings},
number = 1,
volume = 1645,
place = {United States},
year = 2015,
month = 2
}

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