Fast cooling and internal heating in hyperon stars

Anzuini, Filippo; Melatos, A.; Dehman, Clara; Viganò, Daniele; Pons, José A.

doi:10.1093/mnras/stab3126

Cited by 16 publications

(30 citation statements)

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“…While the so-called "hyperon puzzle" has been resolved, other aspects, such as their role in neutrino cooling are just beginning to be studied seriously -see for example Ref. [234]. Their participation in dense matter at the higher temperatures associated with supernovae and the proto-neutron stars formed after neutron star mergers is also a rich area for further study.…”

Section: Discussionmentioning

confidence: 99%

The Role of Baryon Structure in Neutron Stars

Motta,

Thomas

2022

Preprint

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The current state of neutron star mass measurements is depicted in Fig. 1. We see that the only measurements of heavy neutron stars with reasonably small errors are those of PSR J1614-2230 [29] and PSR J0348+0432 [2], along with PSR J0740+6620 [30] which is the newest member of the heavy neutron star club. Nevertheless, the uncertainties on the aforementioned pulsars still make them all comparable with each other within two standard deviations. Therefore, a conservative lower estimate for the maximum mass of neutron stars is that of PSR J1614-2230, namely, 1.908±0.016M . RadiiOther than their masses, the radii of neutron stars are extremely sensitive to different models for the equations of state. However, the experimental constraints on radii are less numerous and until recently the systematic errors were quite large. The first new source of a constraint came on August 17th 2017, with the first gravitational wave measurement [4] of the merger of two neutron stars. This yielded the result that the radii of the neutron stars involved in the merger both lie within R = 11.9 +1.4 −1.4 , at the 90% confidence level.More recently, the NICER mission, with its X-ray telescope on the space station, obtained results [5,37] for PSR J0030+0451. The collaboration applied different analyses on the data and obtained values of (all at 68% credibility) 12.71 +1.14 −1.19 km and mass 1.34 +0.15 −0.16 M in Ref.[5] and 13.02 +1.24 −1.06 km in Ref.[37] with the mass estimated at 1.44 +0.15 −0.14 M . Another recent measurement by the NICER collaboration was that of pulsar PSR J0740+6620 which by virtue of being much heavier, is of considerable interest to nuclear physicists. They measured a radius of 12.39 +1.3 −0.98 km for a mass of 2.07 ± 0.06M [38]. Modelling Dense MatterHistorically, studies of the properties of nuclear matter were primarily aimed at understanding finite nuclei. They were based primarily on using two-body and three-body potentials with standard techniques in quantum many-body theory, such as Brueckner-Hartree-Fock (BHF) [39], Bethe-Brueckner-Goldstone (BBG) [40]. The two-body potentials were derived from phenomenological fits to nucleonnucleon scattering [41]. The quantum Monte Carlo variational approach has had considerable success with light nuclei [42], with parameters of the phenomenological three-body force tuned to nuclear data. In recent years there has been a great deal of activity using chiral effective field theory [43,44,45,46,47,48], with its systematic expansion in powers of momentum. This approach builds in the constraints of chiral symmetry within a Lagrangian theory built upon pion and nucleon degrees of freedom, plus counterterms. With a similar number of parameters to those needed for phenomenological potentials (typically 25-30), it yields a good description of nucleon-nucleon scattering data. Within the same framework, one also has a systematic expansion of a three-nucleon force, with counterterms again tuned to nuclear data. Once again one finds excellent agreement with data for light nuc...

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Section: Discussionmentioning

confidence: 99%

The Role of Baryon Structure in Neutron Stars

Motta,

Thomas

2022

Preprint

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“…The exact timescale of the response to BNV reactions by the weak processes (τ weak ) would depend on the specific reaction, and the temperature of the star. For a general estimate of the timescales involved, let us consider the Urca processes [106] which are extensively studied in the context of neutron star cooling theories [107][108][109]. Direct Urca processes involve baryon -decays and lepton ( = e, µ) capture:…”

Section: General Conditionsmentioning

confidence: 99%

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

2022

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The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.

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“…The exact timescale of the response to BNV reactions by the weak processes (τ weak ) would depend on the specific reaction, and the temperature of the star. For a general estimate of the timescales involved, let us consider the URCA processes [105] which are extensively studied in the context of neutron star cooling theories [106][107][108]. Direct URCA processes involve baryon -decays and lepton ( = e, µ) capture:…”

Section: General Conditionsmentioning

confidence: 99%

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Berryman,

Gardner,

Zakeri

2022

Preprint

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Fast cooling and internal heating in hyperon stars

Cited by 16 publications

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The Role of Baryon Structure in Neutron Stars

The Role of Baryon Structure in Neutron Stars

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

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