Neutron matter - Quark matter phase transition and Quark star
Int.J.Mod.Phys.E2:547-564,1993 We consider the neutron matter quark matter phase transition along with possible existence of hybrid quark stars. The equation of state for neutron matter is obtained using a nonperturbative method with pion dressing of the neutron matter and an analysis similar to tha...
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| Main Authors | , , , |
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| Format | Journal Article |
| Language | English |
| Published |
05.01.1993
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| Subjects | |
| Online Access | Get full text |
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| Abstract | Int.J.Mod.Phys.E2:547-564,1993 We consider the neutron matter quark matter phase transition along with
possible existence of hybrid quark stars. The equation of state for neutron
matter is obtained using a nonperturbative method with pion dressing of the
neutron matter and an analysis similar to that of symmetric nuclear matter. The
quark matter sector is treated perturbatively in the small distance domain. For
bag constant $B^{1/4}$=148 MeV, a first order phase transition is seen. In the
context of neutron quark hybrid stars, Tolman-Oppenheimer-Volkoff equations are
solved using the equations of state for quark matter and for neutron matter
with a phase transition as noted earlier. Stable solutions for such stars are
obtained with the Chandrasekhar limit as 1.58 $M_\odot$ and radius around 10
km. The bulk of the star is quark matter with a thin crust of neutron matter of
less than a kilometer. |
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| AbstractList | Int.J.Mod.Phys.E2:547-564,1993 We consider the neutron matter quark matter phase transition along with
possible existence of hybrid quark stars. The equation of state for neutron
matter is obtained using a nonperturbative method with pion dressing of the
neutron matter and an analysis similar to that of symmetric nuclear matter. The
quark matter sector is treated perturbatively in the small distance domain. For
bag constant $B^{1/4}$=148 MeV, a first order phase transition is seen. In the
context of neutron quark hybrid stars, Tolman-Oppenheimer-Volkoff equations are
solved using the equations of state for quark matter and for neutron matter
with a phase transition as noted earlier. Stable solutions for such stars are
obtained with the Chandrasekhar limit as 1.58 $M_\odot$ and radius around 10
km. The bulk of the star is quark matter with a thin crust of neutron matter of
less than a kilometer. |
| Author | Panda, P. K Parida, B. K Mishra, H Misra, S. P |
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| BackLink | https://doi.org/10.48550/arXiv.nucl-th/9301003$$DView paper in arXiv https://doi.org/10.1142/S0218301393000212$$DView published paper (Access to full text may be restricted) |
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| Snippet | Int.J.Mod.Phys.E2:547-564,1993 We consider the neutron matter quark matter phase transition along with
possible existence of hybrid quark stars. The equation... |
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| Title | Neutron matter - Quark matter phase transition and Quark star |
| URI | https://arxiv.org/abs/nucl-th/9301003 |
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