Astrophysical and Theoretical Physics Implications from Multimessenger Neutron Star Observations

Silva, Hector O.; Holgado, A. M.; Cárdenas-Avendaño, Alejandro; Yunes, Nicolás

doi:10.1103/physrevlett.126.181101

Cited by 115 publications

(87 citation statements)

References 72 publications

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“…Big Bang nucleosynthesis constraints should also be carefully taken into account in the post-inflationary era of the model. We also mention that, so far, there is no observational evidence for the existence of Chern–Simons gravity in the late Universe [99], which is in agreement with the basic feature of our proposed stringy RVM cosmology on the cancellation of gravitational anomalies in the post-inflationary epochs. Phenomenological comparison of our string-inspired cosmological model, which is characterized by a totally antisymmetric torsion, with other cosmologies with torsion (e.g.…”

Section: Discussionsupporting

confidence: 90%

Geometrical origins of the universe dark sector: string-inspired torsion and anomalies as seeds for inflation and dark matter

Mavromatos

2022

Phil. Trans. R. Soc. A.

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In a modest attempt to present potentially new paradigms in cosmology, including its inflationary epoch, and initiate discussions, I review in this article some novel, string-inspired cosmological models, which entail a purely geometrical origin of the dark sector of the Universe but also of its observed matter-antimatter asymmetry. The models contain gravitational (string-model independent, Kalb–Ramond (KR)) axion fields coupled to primordial gravitational anomalies via CP-violating interactions. The anomaly terms are four-space–time-dimensional remnants of the Green–Schwarz counterterms appearing in the definition of the field strength of the spin-one antisymmetric tensor field of the (bosonic) massless gravitational string multiplet, which also plays the role of a totally antisymmetric component of torsion. I show how in such cosmologies the presence of primordial gravitational waves can lead to anomaly condensates and dynamical inflation of a ‘running-vacuum-model’ type, without external inflatons, but also to leptogenesis in the radiation era due to anomaly induced Lorentz and CPT violating KR axion backgrounds. I also discuss how the torsion-related KR-axion could acquire a mass during the QCD epoch, thus playing the role of (a component of) dark matter. Phenomenological considerations of the inflationary and post-inflationary (in particular, modern) eras of the model are briefly discussed, including its potential for alleviating the observed tensions in the cosmological data of the current epoch. This article is part of the theme issue ‘The future of mathematical cosmology, Volume 1’.

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Section: Discussionsupporting

confidence: 90%

Geometrical origins of the universe dark sector: string-inspired torsion and anomalies as seeds for inflation and dark matter

Mavromatos

2022

Phil. Trans. R. Soc. A.

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“…and [17] (see, e.g., Equation (4. Equations ( 40) and (41) correct the wrong range for ω2PN which one would obtain for the Double Pulsar by summing the values in Equation (20) and Equation ( 21) of 6 Iorio [11]. From Figure 2, the 2PN periastron precession of PSR J0737-3039A/B is always retrograde and does not vanish for any value of f 0 .…”

Section: Numerically Integrating the 1pn + 2pn Equations Of Motionmentioning

confidence: 95%

“…In Equation (3), stands for arcseconds. Equation ( 3) is to be compared with the retrograde Lense-Thirring periastron rate which, if calculated with the latest determination of I A by Silva et al [6], would be of comparable magnitude 2 ωLT, A −0.0006 • yr −1 = −2.16 yr −1 . (…”

Section: Introductionmentioning

confidence: 99%

On the 2PN Periastron Precession of the Double Pulsar PSR J0737–3039A/B

Iorio

2021

Universe

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One of the post-Keplerian (PK) parameters determined in timing analyses of several binary pulsars is the fractional periastron advance per orbit kPK. Along with other PK parameters, it is used in testing general relativity once it is translated into the periastron precession ω˙PK. It was recently remarked that the periastron ω of PSR J0737–3039A/B may be used to measure/constrain the moment of inertia of A through the extraction of the general relativistic Lense–Thirring precession ω˙LT,A≃−0.00060∘yr−1 from the experimentally determined periastron rate ω˙obs provided that the other post-Newtonian (PN) contributions to ω˙exp can be accurately modeled. Among them, the 2PN seems to be of the same order of magnitude of ω˙LT,A. An analytical expression of the total 2PN periastron precession ω˙2PN in terms of the osculating Keplerian orbital elements, valid not only for binary pulsars, is provided, thereby elucidating the subtleties implied in correctly calculating it from k1PN+k2PN and correcting some past errors by the present author. The formula for ω˙2PN is demonstrated to be equivalent to that obtainable from k1PN+k2PN by Damour and Schäfer expressed in the Damour–Deruelle (DD) parameterization. ω˙2PN actually depends on the initial orbital phase, hidden in the DD picture, so that −0.00080∘yr−1≤ω˙2PN≤−0.00045∘yr−1. A recently released prediction of ω˙2PN for PSR J0737–3039A/B is discussed.

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“…In several recent studies, the MOI of A has been predicted based on EOSs constrained using physical stability arguments (Raithel et al 2016), NS observations (Steiner et al 2015;Landry & Kumar 2018;Kumar & Landry 2019;Jiang et al 2020;Silva et al 2021), or the results of nuclear experiments (Worley et al 2008;Lim et al 2019). However, a phase transition was not explicitly taken into account in these previous studies.…”

Section: Introductionmentioning

confidence: 99%

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

Miao¹,

Li²

2021

Preprint

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We extend our previous study (Li et al. 2021) on neutron stars with a quark core to predict the moment of inertia of pulsar A in the double pulsar binary J0737-3039, assuming there is a phase transition in the pulsar inner core from the soft QMF or the stiff DD2 hadronic equation of state (EOS) to a high-density phase of quark matter modelled by the generic "constant-sound-speed" (CSS) parameterization. We perform a Bayesian analysis of the moment of inertia by incorporating observational data for the tidal deformability of the GW170817 and GW190425 binary neutron star mergers, as detected by LIGO/Virgo, and the mass and radius of PSR J0030+0451 and MSP J0740+6620, as detected by the Neutron Star Interior Composition Explorer. We find that the most probable values of the moment of inertia of PSR J0737-3039 A are 1.27 +0.18 −0.14 × 10 45 g cm 2 for QMF+CSS and similarly 1.29 +0.26 −0.15 × 10 45 g cm 2 for DD2+CSS at 90% credible interval. We also demonstrate how a moment of inertia measurement would improve our knowledge of the EOS and the mass-radius relation for hybrid stars and discuss whether a quark deconfinement phase transition is supported by the available data and forthcoming data that could be consistent with this hypothesis.

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Astrophysical and Theoretical Physics Implications from Multimessenger Neutron Star Observations

Cited by 115 publications

References 72 publications

Geometrical origins of the universe dark sector: string-inspired torsion and anomalies as seeds for inflation and dark matter

Geometrical origins of the universe dark sector: string-inspired torsion and anomalies as seeds for inflation and dark matter

On the 2PN Periastron Precession of the Double Pulsar PSR J0737–3039A/B

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

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