Hypernuclear matter in strong magnetic field

Sinha, Monika; Mukhopadhyay, Banibrata; Sedrakian, Armen

doi:10.1016/j.nuclphysa.2012.12.076

Cited by 71 publications

(78 citation statements)

References 78 publications

(111 reference statements)

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“…Comparing our work with [36] we show that significant differences on maximum masses and their respective radii for stronger magnetic fields can be obtained depending on the choice of the parameters for slow and fast decays of the density dependent magnetic field. This means that different combinations of parameters can generate controllable values for masses and radii, as expected from the results obtained in [30].…”

Section: Introductionsupporting

confidence: 61%

“…In [30], different profiles for the density dependence of the magnetic field were studied in the context of hadronic stars and the authors concluded that the equation of state is insensitive to magnetic fields lower than 10 18 G, a behaviour already observed in [36,38,39] for different models. Moreover, they found that for magnetic fields higher than 10 18 G, matter becomes unstable due to the increase of anisotropic effects on the pressure.…”

Section: Resultsmentioning

confidence: 94%

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Hadronic and hybrid stars subject to density-dependent magnetic fields

2014

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In the light of the very massive neutron stars recently detected and the new possible constraints for the radii of these compact objects, we revisit some equations of state obtained for hadronic and hybrid stars under the influence of strong magnetic fields. We present our results for hadronic matter taking into account the effects of the inclusion of anomalous magnetic moment. Additionally, the case of hybrid stars under the influence of strong magnetic fields is considered. We study the structure of hybrid stars based on the Maxwell condition (without a mixed phase), where the hadron phase is described by the non-linear Walecka model (NLW) and the quark phase by the Nambu-Jona-Lasinio model (NJL). The mass-radius relation for each case are calculated and discussed. We show that both hadronic and hybrid stars can bear very high masses and radii compatible with the recently observed high mass neutron stars.

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Section: Introductionsupporting

confidence: 61%

Section: Resultsmentioning

confidence: 94%

Hadronic and hybrid stars subject to density-dependent magnetic fields

2014

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“…Over the years, it has been shown that the presence of strong magnetic fields significantly affects the energy levels of charged particles due to Landau quantization. These effects have been taken into account in the EoS of models in order to describe hyperon stars (Chakrabarty et al 1997;Broderick et al 2000Broderick et al , 2002Lopes & Menezes 2012;Sinha et al 2013;Casali et al 2014;Gomes et al 2014;Gao et al 2015), quark stars (Perez Martinez et al 2008;Felipe et al 2011;Orsaria et al 2011;Paulucci et al 2011;Denke & Pinto 2013;Dexheimer et al 2014;Isayev 2015), hybrid stars (Rabhi et al 2009;Dexheimer et al 2012Dexheimer et al , 2013, and stars with meson condensates Schramm et al (2015). The effects of the anomalous magnetic moment (AMM) were also investigated through the corresponding coupling of the baryons to the electromagnetic field tensor (see Canuto & Chiu 1968a;Broderick et al 2000Broderick et al , 2002Strickland et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Many-body Forces in Magnetic Neutron Stars

Gomes

Franzon

Dexheimer

et al. 2017

ApJ

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In this work, we study in detail the effects of many-body forces on the equation of state and the structure of magnetic neutron stars. The stellar matter is described within a relativistic mean field formalism that takes into account many-body forces by means of a nonlinear meson field dependence on the nuclear interaction coupling constants. We assume that matter is at zero temperature, charge neutral, in beta equilibrium, and populated by the baryon octet, electrons, and muons. In order to study the effects of different degrees of stiffness in the equation of state, we explore the parameter space of the model, which reproduces nuclear matter properties at saturation, as well as massive neutron stars. Magnetic field effects are introduced both in the equation of state and in the macroscopic structure of stars by the self-consistent solution of the Einstein-Maxwell equations. In addition, the effects of poloidal magnetic fields on the global properties of stars, as well as density and magnetic field profiles, are investigated. We find that not only different macroscopic magnetic field distributions but also different parameterizations of the model for a fixed magnetic field distribution impact the gravitational mass, deformation, and internal density profiles of stars. Finally, we show that strong magnetic fields significantly affect the particle populations of stars.

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“…However, below the field values 10 18 G the abundances of baryons for non-zero B are indistinguishable from those in the B = 0 case (see Ref. [7] and references therein).…”

Section: Microphysical Inputmentioning

confidence: 98%

Magnetar superconductivity versus magnetism: Neutrino cooling processes

Sinha

Sedrakian

2015

Phys. Rev. C

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We describe the microphysics, phenomenology, and astrophysical implication of a B-field induced unpairing effect that may occur in magnetars, if the local B-field in the core of a magnetar exceeds a critical value Hc2. Using the Ginzburg-Landau theory of superconductivity, we derive the Hc2 field for proton condensate taking into the correction (≤ 30%) which arises from its coupling to the background neutron condensate. The density dependence of pairing of proton condensate implies that Hc2 is maximal at the crust-core interface and decreases towards the center of the star. As a consequence, magnetar cores with homogenous constant fields will be partially superconducting for "medium-field" magnetars (10 15 ≤ B ≤ 5 × 10 16 G) whereas "strong-field" magnetars (B > 5 × 10 16 G) will be void of superconductivity. The neutrino emissivity of a magnetar's core changes in a twofold manner: (i) the B-field assisted direct Urca process is enhanced by orders of magnitude, because of the unpairing effect in regions where B ≥ Hc2; (ii) the Cooper-pair breaking processes on protons vanish in these regions and the overall emissivity by the pair-breaking processes is reduced by a factor of only a few.

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Hypernuclear matter in strong magnetic field

Cited by 71 publications

References 78 publications

Hadronic and hybrid stars subject to density-dependent magnetic fields

Hadronic and hybrid stars subject to density-dependent magnetic fields

Many-body Forces in Magnetic Neutron Stars

Magnetar superconductivity versus magnetism: Neutrino cooling processes

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