Maximum gravitational mass 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msub><mml:mi>M</mml:mi><mml:mrow><mml:mi>TOV</mml:mi></mml:mrow></mml:msub><mml:mo>=</mml:mo><mml:mn>2.2</mml:mn><mml:msubsup><mml:mn>5</mml:mn><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.07</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.08</mml:mn></mml:mrow></mml:msubsup><mml:msub><mml:mi>M</mml:mi><mml:mo stretchy="false">⊙</mml:mo></mml:msub></mml:math>
 inferred at about 3% precision with mul

Fan, Yi-Zhong; Han, Ming-Zhe; Jiang, Jin-Liang; Shao, Dong-Sheng; Tang, Shao-Peng

doi:10.1103/physrevd.109.043052

Cited by 10 publications

(7 citation statements)

References 119 publications

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“…Now the NICER data for PSR J0030+0451 is excluded from the constraints on the NS EOS. To improve the precision of the constraints, we also incorporate the M TOV information derived from the NS mass function by Fan et al (2024) 12.37 0.69 0.50 km). These results are closer to the NICER analysis results using the ST +PDT hot spot model (see Figure 3).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…In the top part of Figure 6, we have also compared the mass distributions of the sources RBS 1223, RX J0720.4-3125, and RX J1856.5-3754 with the probability distribution of masses of the NSs measured in binary systems (i.e., the black solid line, which is adopted from Fan et al 2024). It is found that the masses of these INSs are relatively small (for RX J1856.5-3754, the error bar is quite large because of the poorly constrained z g ), implying that the masses of (some) NSs in binary systems have been significantly increased through accretion.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…In this work, we follow such an approach. To strengthen the constraints on the EOS, we also incorporate the M TOV information inferred from the NS mass function (see Section III.A of Fan et al 2024 for the details).…”

Section: The Data and Information Used In The Eos Reconstructionmentioning

confidence: 99%

“…Unfortunately, in the last two years, neither the LIGO/Virgo collaboration nor the NICER mission has provided new, improved NS M-R measurements. An improvement we present here is the incorporation of NS mass function information following Fan et al (2024), which provides further constraints on the EOS. Unlike Tang et al (2020) and Luo et al (2022), which only took parameterized EOS representation/reconstruction, our approach is based on the EOS (non)parametric reconstruction results using feed-forward neural network (i.e., FFNN; see Han et al 2021Han et al , 2023, flexible piecewise linear sound speed (i.e., PWLS; see Jiang et al 2023), and Gaussian processes (i.e., GP; see Landry et al 2020;Gorda et al 2023) methods.…”

mentioning

confidence: 99%

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Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Luo,

Tang,

Han

et al. 2024

ApJ

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In 2019, the Neutron star Interior Composition ExploreR (NICER) mission released its findings on the mass and radius of the isolated neutron star (INS) PSR J0030+0451, revealing a mass of approximately 1.4 solar masses (M ⊙) and a radius near 13 km. However, the recent reanalysis by the NICER collaboration suggests that the available data primarily yield a precise inference of the compactness for this source while the resulting mass and radius are strongly model-dependent and diverse (the 68.3% credible regions just overlap slightly for the ST+PDT and PDT-U models). By integrating this compactness data with the equation of state (EOS) refined by our latest investigations, we have deduced the mass and radius for PSR J0030+0451, delivering estimates of M = 1.48 − 0.10 + 0.09 M ⊙ and R = 12.38 − 0.70 + 0.51 km for the compactness found in the ST+PDT model, alongside M = 1.47 − 0.20 + 0.14 M ⊙ and R = 12.37 − 0.69 + 0.50 km for the compactness in the PDT-U model. These two groups of results are well consistent with each other and the direct X-ray data inference within the ST+PDT model seems to be favored. Additionally, we have calculated the tidal deformability, moment of inertia, and gravitational binding energy for this neutron star. Furthermore, employing these refined EOS models, we have updated mass–radius estimates for three INSs with established gravitational redshifts.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Section: Conclusion and Discussionmentioning

confidence: 99%

Section: The Data and Information Used In The Eos Reconstructionmentioning

confidence: 99%

mentioning

confidence: 99%

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Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Luo,

Tang,

Han

et al. 2024

ApJ

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“…Since compactness and mass accretion rate are tightly aligned and the mass accretion rate is the primary factor in the accumulated mass of the residue of collapse, this relationship is a natural prediction of the neutrino-driven mechanism of CCSNe. With this derived relationship between compactness and gravitational mass, one can use the compactness/ZAMS mass correlation (itself a function of the provenance of the progenitor models) to derive a birth mass function for neutron stars (Özel & Freire 2016;Fan et al 2024;Vartanyan et al 2023). This should be a program for future work.…”

Section: Neutron Star Massmentioning

confidence: 99%

Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory

Burrows,

Wang,

Vartanyan

2024

ApJL

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In this paper, we derive correlations between core-collapse supernova observables and progenitor core structures that emerge from our suite of 20 state-of-the-art 3D core-collapse supernova simulations carried to late times. This is the largest such collection of 3D supernova models ever generated and allows one to witness and derive testable patterns that might otherwise be obscured when studying one or a few models in isolation. From this panoramic perspective, we have discovered correlations between explosion energy, neutron star gravitational birth masses, 56Ni and α-rich freezeout yields, and pulsar kicks and theoretically important correlations with the compactness parameter of progenitor structure. We find a correlation between explosion energy and progenitor mantle binding energy, suggesting that such explosions are self-regulating. We also find a testable correlation between explosion energy and measures of explosion asymmetry, such as the ejecta energy and mass dipoles. While the correlations between two observables are roughly independent of the progenitor zero-age main-sequence (ZAMS) mass, the many correlations we derive with compactness cannot unambiguously be tied to a particular progenitor ZAMS mass. This relationship depends on the compactness/ZAMS mass mapping associated with the massive star progenitor models employed. Therefore, our derived correlations between compactness and observables may be more robust than with ZAMS mass but can nevertheless be used in the future once massive star modeling has converged.

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Strong gravity extruding peaks in speed of sound profiles of massive neutron stars

Cai,

2024

Phys. Rev. D

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Maximum gravitational mass MTOV=2.25−0.07+0.08M⊙ inferred at about 3% precision with mul

Cited by 10 publications

References 119 publications

Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Bulk Properties of PSR J0030+0451 Inferred with the Compactness Measurement of NICER

Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory

Strong gravity extruding peaks in speed of sound profiles of massive neutron stars

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