Results of the summarizing process for the arXiv paper: 2309.12644v1

The maximal gravitational mass of nonrotating neutron stars ($M_{\rm TOV}$) is a crucial parameter in understanding compact objects. However, setting precise bounds on $M_{\rm TOV}$ based on first principles alone is challenging. In this study, the authors leverage reliable measurements of neutron star masses and/or radii to robustly infer $M_{\rm TOV}$. By combining the mass distribution of these objects with the reconstruction of the equation of state (EoS) of dense matter, they achieve a precise inference of $M_{\rm TOV}=2.25^{+0.08}_{-0.07}~M_\odot$ with 68.3% credibility. To obtain this result, the authors utilize various data sources, including an updated sample of neutron star mass measurements, mass-tidal deformability data from GW170817, and mass-radius data from PSR J0030+0451 and PSR J0740+6620. They also incorporate theoretical information from chiral effective theory ($\chi$EFT) and perturbative quantum chromodynamics (pQCD) at low and very high energy densities respectively. The narrow credible range for $M_{\rm TOV}$ obtained in this study is attributed to two factors. Firstly, the high $M_{\rm TOV}$ values are suppressed by the pQCD constraint derived from theoretical considerations. Secondly, lower values of $M_{\rm TOV}$ are excluded by the mass function. To ensure robustness in their findings, three different EoS reconstruction methods are employed independently leading to almost identical results for $M_{\rm TOV}$. This precise evaluation suggests that the equation of state for neutron star matter is moderately stiff. Furthermore, based on their findings, the authors propose that compact objects detected by second-generation gravitational wave detectors with masses around $\sim 2.5-3 M_\odot$ are most likely lightest black holes rather than neutron stars. Overall this study provides a refined and detailed understanding of the maximal gravitational mass of nonrotating neutron stars highlighting the importance of combining multiple data sources and theoretical considerations to obtain precise inferences.

• The maximal gravitational mass of nonrotating neutron stars ($M_{\rm TOV}$) is a crucial parameter in understanding compact objects.
• Precise bounds on $M_{\rm TOV}$ based on first principles alone are challenging.
• Reliable measurements of neutron star masses and/or radii are leveraged to infer $M_{\rm TOV}$ in this study.
• $M_{\rm TOV}=2.25^{+0.08}_{-0.07}~M_\odot$ with 68.3% credibility is obtained by combining the mass distribution of neutron stars with the reconstruction of the equation of state (EoS) of dense matter.
• Various data sources, including updated neutron star mass measurements, GW170817 data, and PSR J0030+0451 and PSR J0740+6620 data, are utilized.
• Theoretical information from chiral effective theory ($\chi$EFT) and perturbative quantum chromodynamics (pQCD) is incorporated at low and very high energy densities respectively.
• The narrow credible range for $M_{\rm TOV}$ is attributed to pQCD constraints and exclusion by the mass function.
• Three different EoS reconstruction methods lead to almost identical results for $M_{\rm TOV}$, ensuring robustness in the findings.
• The equation of state for neutron star matter is moderately stiff based on this precise evaluation.
• Compact objects detected by second-generation gravitational wave detectors with masses around $\sim 2.5-3 M_\odot$ are most likely lightest black holes rather than neutron stars according to the authors' proposal.
• Combining multiple data sources and theoretical considerations is important for obtaining precise inferences about the maximal gravitational mass of nonrotating neutron stars.

Summary: Scientists have been trying to understand how heavy neutron stars can get. It is difficult to figure out the maximum weight of these stars using only basic principles. In this study, scientists used measurements of neutron star masses and sizes to estimate the maximum weight. They found that the maximum weight is about 2.25 times the mass of our Sun. They used different types of data and theories to make sure their findings were accurate. The scientists also discovered that objects with masses around 2.5-3 times the mass of our Sun are more likely to be black holes than neutron stars. Definitions- Neutron stars: Very dense and compact objects in space made mostly of neutrons. - Gravitational mass: The measure of how much an object weighs due to gravity. - Nonrotating: Not spinning or rotating. - Credibility: How believable or trustworthy something is. - Equation of state (EoS): A mathematical description that tells us how matter behaves under different conditions. - Data sources: Different types of information or evidence used for research. - Chiral effective theory (χEFT): A type of theory used in physics to describe interactions between particles at low energy densities. - Perturbative quantum chromodynamics (pQCD): A type of theory used in physics to describe interactions between particles at very high energy densities. - Mass function: A mathematical function that describes the distribution or range of masses for a group of objects. - Robustness: How strong or reliable

Maximal Gravitational Mass of Nonrotating Neutron Stars: A Precise Evaluation

Neutron stars are some of the most fascinating objects in the universe. These ultra-dense stellar remnants, formed after a supernova explosion, have masses comparable to that of our Sun but sizes similar to those of large cities. The maximal gravitational mass of nonrotating neutron stars ($M_{\rm TOV}$) is an important parameter for understanding these compact objects and their properties. However, setting precise bounds on $M_{\rm TOV}$ based on first principles alone is challenging.

In this study, researchers leverage reliable measurements of neutron star masses and/or radii to robustly infer $M_{\rm TOV}$. By combining the mass distribution of these objects with the reconstruction of the equation of state (EoS) for dense matter, they achieve a precise evaluation with 68.3% credibility resulting in $M_{\rm TOV}=2.25^{+0.08}_{-0.07}~M_\odot$. To obtain this result, various data sources were utilized including an updated sample of neutron star mass measurements as well as mass-tidal deformability data from GW170817 and mass-radius data from PSR J0030+0451 and PSR J0740+6620. In addition, theoretical information from chiral effective theory ($\chi$EFT) and perturbative quantum chromodynamics (pQCD) at low and very high energy densities respectively was also incorporated into their analysis.

The narrow credible range for $M_{\rm TOV}$ obtained in this study can be attributed to two factors; Firstly, high values are suppressed by pQCD constraints derived from theoretical considerations while lower values are excluded by the mass function itself due to lack observational evidence for such low masses among known neutron stars. To ensure robustness in their findings three different EoS reconstruction methods were employed independently leading to almost identical results for $M_{\rm TOV}$. This suggests that the equation of state for neutron star matter is moderately stiff which has implications regarding its composition and structure when under extreme conditions such as those found within a neutron star's core region where temperatures reach up to billions degrees Celsius and pressures exceed those found at Earth's core by several orders magnitude!

Based on their findings authors propose that compact objects detected by second-generation gravitational wave detectors with masses around $\sim 2.5-3 M_\odot$ are most likely lightest black holes rather than neutron stars since it would be highly unlikely for any known mechanism or process to produce a nonrotating neutron star above this limit given its already constrained maximal gravitational mass value according to this research paper's findings!

Overall this study provides a refined understanding about the maximal gravitational mass limits set upon nonrotating neutron stars highlighting how combining multiple data sources along with theoretical considerations can lead us towards more precise inferences about these exotic astrophysical entities!