We introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities and a set of stiff quark matter EoS at high densities within a finite region of chemical potentials $μ_H < μ< μ_Q$. Fixing the hadronic EoS as the APR one and choosing the color-superconducting, nonlocal NJL model with two free parameters for the quark phase, we perform Bayesian analyses with this two-parameter family of hybrid EoS. Using three different sets of observational constraints that include the mass of PSR J0740+6620, the tidal deformability for GW170817, and the mass-radius relation for PSR J0030+0451 from NICER as obligatory (set 1), while set 2 uses the possible upper limit on the maximum mass from GW170817 as an additional constraint and set 3 instead of the possibility that the lighter object in the asymmetric binary merger GW190814 is a neutron star. We confirm that in any case, the quark matter phase has to be color superconducting with the dimensionless diquark coupling approximately fulfilling the Fierz relation $η_D=0.75$ and the most probable solutions exhibiting a proportionality between $η_D$ and $η_V$, the coupling of the repulsive vector interaction that is required for a sufficiently large maximum mass. We used the Bayesian analysis to investigate with the method of fictitious measurements the consequences of anticipating different radii for the massive $2~M_\odot$ PSR J0740+6220 for the most likely equation of state. With the actual outcome of the NICER radius measurement on PSR J0740+6220 we could conclude that for the most likely hybrid star EoS would not support a maximum mass as large as $2.5~M_\odot$ so that the event GW190814 was a binary black hole merger.
NS-UNO: Neutron Star EoS Inference from an Unconstrained Number of Observations
University of Coimbra（科英布拉大学）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）；INFN Sezione di Ferrara（费拉拉意大利国家核物理研究所）
From Multimessenger Inference to Simulations: A Ranked Ensemble of Finite-Temperature Equations of State
Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena（耶拿弗里德里希·席勒大学理论物理研究所）；Institute for Gravitation and the Cosmos, The Pennsylvania State University（宾夕法尼亚州立大学引力与宇宙学研究所）；Department of Physics, The Pennsylvania State University（宾夕法尼亚州立大学物理系）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文学与天体物理学系）
Constraints on the dense matter equation of state and neutron star properties from NICER's mass-radius estimate of PSR J0740+6620 and multimessenger observations
The impact of nuclear equations of state on the dynamics and multi-messenger emission of magnetorotational stellar explosions
Università di Firenze（佛罗伦萨大学）；INAF, Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INFN, Sezione di Firenze（意大利国家核物理研究所佛罗伦萨分部）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理研究所）；Sorbonne Université（索邦大学）；Universitat de València（瓦伦西亚大学）；Observatori Astronòmic, Universitat de València（瓦伦西亚大学天文观测站）
A Partially Supervised Latent-Space Variational Autoencoder for Generating Neutron Star Equations of State
University of California, Berkeley（加州大学伯克利分校）；Institute for Nuclear Theory, University of Washington（华盛顿大学核理论研究所）；Amazon Science（亚马逊科学）；Stony Brook University（石溪大学）
Hyperonic compact stars with vector portal dark matter
Utkal University（乌塔卡尔大学）；University of Coimbra（科英布拉大学）；Indian Institute of Science Education and Research Berhampur（印度科学教育研究学院贝尔汉普尔分校）；National Institute of Science Education and Research（国家科学教育研究中心）；Homi Bhabha National Institute（霍米·巴巴国立研究所）；Institute of Physics Bhubaneswar（布巴内斯瓦尔物理研究所）；Indian Institute of Technology Bhilai（印度理工学院比莱分校）
Bayesian Inference of Dense-Matter Equations of State from Small-Radius Compact Stars with Twin-Star Scenarios
School of Physics, Nankai University（南开大学物理学院）；Shenzhen Research Institute of Nankai University（南开大学深圳研究院）；Department of Physics, Faculty of Science, Tianjin University（天津大学理学院物理系）
本文通过贝叶斯方法研究致密物质方程 of state，探讨小半径致密星体是否能被双星情景所容纳，通过约束参数发现相变特征及对潮汐变形性的影响。
Extending multi-messenger constraints on neutron star matter through the inclusion of direct Urca cooling
Universität Potsdam（波茨坦大学）；National Research and Innovation Agency (BRIN)（国家研究与创新署）；Utrecht University（乌得勒支大学）；Nikhef（尼赫夫）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））
Rotational enhancement and stability of protoquark stars during thermal evolution
Instituto Tecnológico de Aeronáutica（航空技术学院）；Laboratório de Computação Científica Avançada e Modelamento (Lab-CCAM)（先进计算与建模实验室）；University of Coimbra（科英布拉大学）；University of Cyprus（塞浦路斯大学）；The Cyprus Institute（塞浦路斯研究所）；Yonsei University（延世大学）
Universal description of the Neutron Star's surface and its key global properties: A Machine Learning Approach for nonrotating and rapidly rotating stellar models
Universal relations for hybrid stars and their quark cores: a systematic scan of the quark-matter parameter space
Universidad Nacional de La Plata（拉普拉塔国立大学）；CONICET（阿根廷国家科学研究委员会）；Instituto de Astronomía y Física del Espacio (IAFE, CONICET-UBA)（天文与空间物理研究所 (IAFE, 阿根廷国家科学研究委员会-布宜诺斯艾利斯大学)）；Universidade Federal do ABC（ABC联邦大学）
Needle in a Bayes Stack: a Hierarchical Bayesian Method for Constraining the Neutron Star Equation of State with an Ensemble of Binary Neutron Star Post-merger Remnants
A self-consistent single-fluid framework for neutron stars admixed with mirror dark matter
University of Coimbra（科英布拉大学）；Instituto Tecnológico de Aeronáutica（航空技术学院）；Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）；University of Tübingen（蒂宾根大学）
