Equation of State of Strongly Magnetized Matter with Hyperons and Δ-Resonances

Thapa, Vivek Baruah; Sinha, Monika; Li, Jia Jie; Sedrakian, Armen

doi:10.3390/particles3040043

Cited by 33 publications

(19 citation statements)

References 51 publications

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“…Regarding the effect of the strong MF, we find that not always the magnetar models have a higher maximum mass than the low MF models, unlike other works (Rabhi et al 2009;Mariani et al 2019;Thapa et al 2020;Rather et al 2021); in our model, Sets 1 and 2 show slightly higher maximum masses for magnetars, but for Set 3 3 for details).…”

Section: Results For Stellar Structure and Stabilitycontrasting

confidence: 66%

Oscillating magnetised hybrid stars under the magnifying glass of multi-messenger observations

Mariani,

Tonetto,

Rodríguez

et al. 2022

Preprint

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We model neutron stars as magnetised hybrid stars with an abrupt hadron-quark phase transition in their cores, taking into account current constraints from nuclear experiments and multi-messenger observations. We include magnetic field effects considering the Landau level quantisation of charged particles and the anomalous magnetic moment of neutral particles. We construct the magnetised hybrid equation of state, and we compute the particle population, the matter magnetisation and the transverse and parallel pressure components. We integrate the stable stellar models, considering the dynamical stability for rapid or slow hadron-quark phase conversion. Finally, we calculate the frequencies and damping times of the fundamental and 𝑔 non-radial oscillation modes. The latter, a key mode to learn about phase transitions in compact objects, is only obtained for stars with slow conversions. For low magnetic fields, we find that one of the objects of the GW170817 binary system might be a hybrid star belonging to the slow extended stability branch. For magnetars, we find that a stronger magnetic field always softens the hadronic equation of state. Besides, only for some parameter combinations a stronger magnetic field implies a higher hybrid star maximum mass. Contrary to previous results, the incorporation of anomalous magnetic moment does not affect the studied astrophysical quantities. We discuss possible imprints of the microphysics of the equation of state that could be tested observationally in the future, and that might help infer the nature of dense matter and hybrid stars.

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Section: Results For Stellar Structure and Stabilitycontrasting

confidence: 66%

Oscillating magnetised hybrid stars under the magnifying glass of multi-messenger observations

Mariani,

Tonetto,

Rodríguez

et al. 2022

Preprint

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“…For the inclusion of these effects see Refs. [42][43][44]. We do not consider in this work the non-strange J = 3 2 members of the baryons decuplet-the ∆-resonances [35,[45][46][47][48][49][50]; for a review, see [21].…”

Section: Equation Of Statementioning

confidence: 99%

Equation of State and Composition of Proto-Neutron Stars and Merger Remnants with Hyperons

Sedrakian

Harutyunyan

2021

Universe

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Finite-temperature equation of state (EoS) and the composition of dense nuclear and hypernuclear matter under conditions characteristic of neutron star binary merger remnants and supernovas are discussed. We consider both neutrino free-streaming and trapped regimes which are separated by a temperature of a few MeV. The formalism is based on covariant density functional (CDF) theory for the full baryon octet with density-dependent couplings, suitably adjusted in the hypernuclear sector. The softening of the EoS with the introduction of the hyperons is quantified under various conditions of lepton fractions and temperatures. We find that Λ, Ξ−, and Ξ0 hyperons appear in the given order with a sharp density increase at zero temperature at the threshold being replaced by an extended increment over a wide density range at high temperatures. The Λ hyperon survives in the deep subnuclear regime. The triplet of Σs is suppressed in cold hypernuclear matter up to around seven times the nuclear saturation density, but appears in significant fractions at higher temperatures, T≥20 MeV, in both supernova and merger remnant matter. We point out that a special isospin degeneracy point exists where the baryon abundances within each of the three isospin multiplets are equal to each other as a result of (approximate) isospin symmetry. At that point, the charge chemical potential of the system vanishes. We find that under the merger remnant conditions, the fractions of electron and μ-on neutrinos are close and are about 1%, whereas in the supernova case, we only find a significant fraction (∼10%) of electron neutrinos, given that in this case, the μ-on lepton number is zero.

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“…The exponential profile of Equation ( 14), although not physically consistent, is a suitable choice to study bulk properties such as the structure and composition of these compact objects since it allows covering a wide range of MF values. Although hypothetical, this exponential parametrization has been used in several works and is an acceptable approximation to model the complex and still unknown profile of the MF (Bandyopadhyay et al, 1997;Mao et al, 2003;Rabhi et al, 2009;Dexheimer et al, 2012;Flores et al, 2020;Thapa et al, 2020;Mariani et al, 2022).…”

Section: Magnetized Strange Quark Matter Within the Mit Bag Modelmentioning

confidence: 99%

Oscillating Magnetized Color Superconducting Quark Stars

Celi,

Mariani,

Orsaria

et al. 2022

Preprint

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The main objective of this work is to study the structure, composition, and oscillation modes of color superconducting quark stars with intense magnetic fields. We adopted the MIT bag model within the color superconductivity CFL framework, and we included the effects of strong magnetic fields to construct the equation of state of stable quark matter. We calculated observable quantities, such as the mass, radius, frequency, and damping time of the oscillation fundamental f mode of quark stars, taking into account current astrophysical constraints. The results obtained show that color superconducting magnetized quark stars satisfy the constraints imposed by the observations of massive pulsars and gravitational wave events. Furthermore, the quantities associated with the oscillation f mode of these objects fit the universal relationships for compact objects. In the context of the new multi-messenger gravitational wave astronomy era and the future asteroseismology of neutron stars, we hope that our results contribute to the understanding of the behavior of dense matter and compact objects.

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Equation of State of Strongly Magnetized Matter with Hyperons and Δ-Resonances

Cited by 33 publications

References 51 publications

Oscillating magnetised hybrid stars under the magnifying glass of multi-messenger observations

Oscillating magnetised hybrid stars under the magnifying glass of multi-messenger observations

Equation of State and Composition of Proto-Neutron Stars and Merger Remnants with Hyperons

Oscillating Magnetized Color Superconducting Quark Stars

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