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Metastability of Hadronic Compact Stars

Metastability of Hadronic Compact Stars. I. Vidaña & I. Bombaci, P. K. Panda, C. Provid ência. “The Complex Physics of Compact Stars” Ladek Zdroj, Poland, 24-29 February 2008. arXiv:0802.1794; PRD in press. In this work:.

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Metastability of Hadronic Compact Stars

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  1. Metastability of Hadronic Compact Stars I. Vidaña & I. Bombaci, P. K. Panda, C. Providência “The Complex Physics of Compact Stars” Ladek Zdroj, Poland, 24-29 February 2008 arXiv:0802.1794; PRD in press

  2. In this work: • We perform a systematic study of the metastability of pure hadronic compact stars with respect to the conversion to quarkstars using different relativistic models for the hadronic EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). • We explore the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, finding that the increase of the hyperon coupling shift the bulk transition point for quark deconfinement to higher densities and makes the conversion to quark stars less likely. • For the QMC model, the formation of a quark star is only possible with a soft quark matter EoS. • Both QMC and GM1 with the largest hyperon-meson couplings predict critical masses which may be as high as 1.9-2.1 M, compatible with highly massive compact stars, suchs as the of the millisecond pulsar PSR B1516+02B and nearly the one PSR J1748-2021B.

  3. Astrophysical Scenario

  4. Nucleation of quark matter in neutron stars has been studied by many authors, due to its potential connection with explosive events such as supernovae and gamma-ray bursts. • Thermal nucleation: (Horvath et al.,1994; Olesen & Madsen 2004; Benvenuto & Lugones 1999) The prompt formation of a critical-size drop of QM via thermal activation is possible for T > 2-3 MeV Pure hadronic stars are converted to quark stars within the first seconds after their birth. However, neutrino trapping in the protoneutron star phase strongly precludes the formation of a quark matter phase • Quantum nucleation:(Grassi 1998; Iida & Sato 1998, Berezhiani et al., 2003, Bombaci et al., • 2004, Drago et al., 2004) It is possible that the star survives the early stages of its evolution as a pure hadronic star. In this case, nucleation of QM would be triggered by quantum fluctuations in degenerate (T=0) neutrino-free hadronic matter.

  5. Formation of a quark matter bubble at the centre of a Neutron Star (I) -stable quark-matter bubble • Direct nucleation of the -stable quark matter: high order weak processsuppressed by a factor ~ GF2N/3, with N=100-1000. Hadron matter Ruled out: even when the final state has a lower energy Berezhiani et al. 2003 (unpaired) Drago, Lavagno & Pagliara 2004 (CFL)

  6. Formation of a quark matter bubble at the centre of a Neutron Star (II) W ~ 10-8 s S~ 10-23 s -stable quark-matter bubble Hadron matter Non--stable quark-matter bubble Q* (Non- stable) Q* (Non- stable) Has the intermediate phaselower energythan hadron matter ?

  7. The intermediate non -stable quark phase • Each flavor is color neutral • Flavor is conserved Iida & Sato 1998 ; Bombaci, Parenti & Vidaña 2004

  8. Lifshitz-Kagan quantum nucleation theory Quantum fluctuation of a virtual drop of QM in HM

  9. Nucleation Time Oscillation frequency of the virtual drop inside the potential well and Penetrability of the potential barrier (WKB) Action over and under the barrier Nucleation time

  10. Critical mass of metastable hadronic stars Definition: Mcr = MHS(= 1 yr) Hadronic stars with MHS< Mcrare metastable with  = 1 yr to infinity Hadronic stars with MHS> Mcrare very unlikely observed “The critical mass Mcrplays the role of an effective maximum mass for the hadronic branch of compact stars” Berezhiani et al. 2003 ; Bombaci et al. 2004

  11. Few words on the EoS considered … • Non Linear Walecka Model We use the Glendenning-Moszkowski (GM) parametrizations GM1 & GM3 of the NLWM (PRL 67, 2414 (1991)), where the hyperon-nucleon couplings, xgY/gN  xgY/gNandxgY/gN, are constrained by the binding of the  hyperon in nuclear matter Neutron star masses, in addition, restrict x to the range 0.6 - 0.8. Here, we will take xx and will consider x=0.6, 0.7, 0.8. • Quark Meson Coupling Model Baryons described as a system of non-overlaping spherical bags containing three valence quarks interacting by the exchange of ,  and  mesons coupled directly to the confined quarks. (PLB 200, 235 (1988)). Here we will take x0.7,x=0.78 and xis an output of the model ~ 0.7. • Quark phase: MIT bag model (Farhi & Jaffe, PRD 30, 2379 (1984))

  12. Hadronic Equation of State • Higher value of the hyperon couplings stiffer EoS. • Onset of hyperons at higher densities for larger values of the couplings. • QMC EoS softer/stiffer than NLWM.

  13. Gibbs free energy & bulk transition point for quark deconfinement The lower the values of hyperon couplings, the softer the EoS and the lower the pressure P0 at the crossing between the hadronic and the Q* phase lower critical masses for smaller hyperon coupling values.

  14. Stable, mestastable and unstable hadron star configurations (I) QMC NLWM (GM1) =30 MeV/fm2 Very narrow metastability region for QMC. The formation of a quark star is only possible in this model for a soft quark matter EoS (i.e., for small values of B).

  15. Stable, mestastable and unstable hadron star configurations (II) NLWM (GM1) QMC • When Mcr star is almost on the top of P0, these stars lie on or close to the plateau that contains the maximum mass configuration. • A large separation between these two configurations corresponds to a phase transition which occurs during the rise of the MP curve before the plateau.

  16. Bag cosnatnt Critical Mass NLWM (GM1) Critical Mass Hyperon coupling Large critical masses due to the softness of the QMC EoS QMC

  17. M=2.081 M, R=12.6 km, fY,cr ~ 30%, RY ~ 8.7 km. Compatible with highly-massive compact stars, such as the one associated to the millisecond pulsar PSR B1516+02B (1.94(+0.17-0.19) M (1)) , and nearly the one PSR J1748-2021B (2.74 (+0.41-0.51) M (2))

  18. Summary & Conclusions4564) We have performed a systematic study of the metastability of pure hadronic compact stars with respect to the conversion to quark stars using different relativistic models for the EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). We have explored the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, finding that the increase of the hyperon coupling shift the bulk transition point for quark deconfinement to higher densities and makes the conversion to quark stars less likely. For the QMC model,the metastability region is very narrow. The EoS is very sofy and therefore the onset of hyperons occurs at quite high densities, which gives rise to large critical masses. The converstion to a quark star will occur only for a small value of the bag constant. Both QMC and GM1 with the largest hyperon-meson couplings predict critical masses which may be as high as 1.9-2.1 M, compatible with the masses of the millisecond pulsar PSR B1516+02B and nearly the one PSR J1748-2021B

  19. Time for Coffee & Cookies Thanks a lot for your patience

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