Accretion‐induced collapse to third family compact stars as trigger for eccentric orbits of millisecond pulsars in binaries

Alvarez-Castillo, David; Antoniadis, John; Ayriyan, Alexander; Blaschke, D.; Danchev, Victor I.; Grigorian, H.; Largani, Noshad Khosravi; Weber, Fridolin

doi:10.1002/asna.201913752

Cited by 10 publications

(9 citation statements)

References 46 publications

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“…The latter case has been recently proposed as an explanation for eccentric orbits of binary systems where the neutron star is able to accrete matter from a circumbinary disk created after a low-mass X-ray episode. Consequently, the neutrino burst which accompanies the deconfinement phase transition in the neutron star interior may trigger a pulsar kick producing the observed eccentric orbit [136]. A pair of compact stars of about the same mass, each one of them lying in different branches of their mass-radius relation are usually called "twin stars", see [137][138][139].…”

Section: Neutron Star Collapse To Third Familymentioning

confidence: 99%

Cosmic-Ray Extremely Distributed Observatory

et al. 2020

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The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a newly formed, global collaboration dedicated to observing and studying cosmic rays (CR) and cosmic-ray ensembles (CRE): groups of at least two CR with a common primary interaction vertex or the same parent particle. The CREDO program embraces testing known CR and CRE scenarios, and preparing to observe unexpected physics, it is also suitable for multi-messenger and multi-mission applications. Perfectly matched to CREDO capabilities, CRE could be formed both within classical models (e.g., as products of photon–photon interactions), and exotic scenarios (e.g., as results of decay of Super-Heavy Dark Matter particles). Their fronts might be significantly extended in space and time, and they might include cosmic rays of energies spanning the whole cosmic-ray energy spectrum, with a footprint composed of at least two extensive air showers with correlated arrival directions and arrival times. As the CRE are predominantly expected to be spread over large areas and, due to the expected wide energy range of the contributing particles, such a CRE detection might only be feasible when using all available cosmic-ray infrastructure collectively, i.e., as a globally extended network of detectors. Thus, with this review article, the CREDO Collaboration invites the astroparticle physics community to actively join or to contribute to the research dedicated to CRE and, in particular, to pool together cosmic-ray data to support specific CRE detection strategies.

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Section: Neutron Star Collapse To Third Familymentioning

confidence: 99%

Cosmic-Ray Extremely Distributed Observatory

et al. 2020

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“…It has been shown that this type of energetic events might have an imprint on the properties of the trajectories of binary systems, whose large eccentricities can be explained by a pulsar kick following the transition without disrupting the system (Alvarez‐Castillo et al 2019a). This transition is also expected to occur in the evolution of the remnant of a compact star merger during the process of formation of a more massive hybrid star or a black hole.…”

Section: Results and Conclusionmentioning

confidence: 99%

“…The argumentation is based on realistic, hadronic EoS calculations that consider baryon-baryon two-body and three-body interactions featuring a repulsive short-range multipomeron exchange potential, resulting in larger compact stars (Yamamoto et al 2016;Yamamoto et al 2017). It has been shown that this type of energetic events might have an imprint on the properties of the trajectories of binary systems, whose large eccentricities can be explained by a pulsar kick following the transition without disrupting the system (Alvarez-Castillo et al 2019a). This transition is also expected to occur in the evolution of the remnant of a compact star merger during the process of formation of a more massive hybrid star or a black hole.…”

Section: F I G U R Ementioning

confidence: 99%

The energy budget of the transition of a neutron star into the third family branch

Alvarez-Castillo

2021

Astron Nachr

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Transition of a compact star into the third family for an equation of state (EoS) featuring mass twins is considered. The energy released at a baryon number conserving the transition of static compact stars configurations is computed for two sets of models for comparison. The EoS of choice is the density-dependent functional DD2 EoS with excluded model corrections for hadronic matter, which suffers a phase transition into deconfined quark matter described by a constant speed of sound approach. The two sets of EoS models feature different compact star mass onsets that maximize the energy and radius difference at the transition while simultaneously fulfilling state-of-the-art constraints from multimessenger astronomy and empirical nuclear data. The maximal energy budget at the transitions was found to fall in the range of 10 49 − 10 52 ergs.

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“…It is also deduced that in the case of the LOCV (AV 18 +TNI) approach, neither CIII nor CIV can meet all the mentioned limits. An astrophysical application of a category CIII EoS based on multiple polytropes can be found in [64] whereas for the CSS EoS is found in [65].…”

Section: Discussionmentioning

confidence: 99%

Studying VLOCV twin compact stars with binary mergers

Sharifi,

Bigdeli,

Alvarez-Castillo

2021

Preprint

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GW170817 has provided valuable constraints on the equations of state of merging binary neutron stars, which can be considered as the most probable candidate for the source of gravitational waves.On the other hand, these natural laboratories of extreme temperature and density may lead to the estimation of some exotic matter like deconfined quark matter in their cores. In this paper, we investigate the neutron star matter equation of state (EoS) with the lowest order constrained variational (LOCV) method considering the excluded volume effect (VLOCV) for nucleons to compute the tidal deformability of binary neutron star mergers (BNSMs). Within this approach, the size of nucleons makes the EoS so stiff that requires a phase transition in order to avoid causality violation. Therefore, this phase transition may lead to the appearance of the third family of compact stars including "twin star" configurations. Our EoS models are confronted with observations from GW170817, GW190814, GW190425, and also NICER. We find out that regarding all these constraints, the EoS models having the transition pressure≈30-100 MeV/fm 3 and the energy density discontinuity ∆ε < ∼ 300 MeV/fm 3 are preferable.

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Accretion‐induced collapse to third family compact stars as trigger for eccentric orbits of millisecond pulsars in binaries

Cited by 10 publications

References 46 publications

Cosmic-Ray Extremely Distributed Observatory

Cosmic-Ray Extremely Distributed Observatory

The energy budget of the transition of a neutron star into the third family branch

Studying VLOCV twin compact stars with binary mergers

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