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Mass Distribution and “Mass Gap” of Compact Stellar Remnants in Binary Systems

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Abstract—The highest critical mass of neutron stars (NSs) was reviewed in the context of equation of state and observational results. It was predicted that the maximum NS mass (\({{M}_{{{\text{NS}}}}}\)) exists in the range \({{M}_{{{\text{NS}}}}} \approx 2.2\)–\(2.9{\kern 1pt} {{M}_{ \odot }}\). However, recent observations of gravitational waves and other studied had suggested the higher mass limit of NSs, \({{M}_{{{\text{NS}}}}} \approx 3.2{\kern 1pt} {{M}_{ \odot }}\). The NS mass upto the value of \({{M}_{{{\text{NS}}}}} \approx 2{\kern 1pt} {{M}_{ \odot }}\) is well understood, and with such a mass value it was meaningful to discuss the “mass gap” (m-gap) between the NS and black hole (BH) collapsars. The “m-gap” exist in between the highest mass of NS and the lowest mass of BH collapsars (\({{M}_{{{\text{m-gap}}}}} \approx 2\)–\(5{\kern 1pt} {{M}_{ \odot }}\)). In the mass distribution, the maximum population of NSs and BHs is located at \({{M}_{{{\text{NS}}}}} = 1.4{\kern 1pt} {{M}_{ \odot }}\) and \({{M}_{{{\text{BH}}}}} = 6.7{\kern 1pt} {{M}_{ \odot }}\), respectively. However, recent observational results predicted filling the “m-gap” by the compact objects. In this paper, the concept of gravidynamics was reported to resolve the problem of peak likelihood value of gravitational mass at \({{M}_{{{\text{peak}}}}} = 6.7{\kern 1pt} {{M}_{ \odot }}\) and the “m-gap” (\({{M}_{{{\text{m-gap}}}}} \approx 2\)–\(5{\kern 1pt} {{M}_{ \odot }}\)). This concept was based on a non-metric scalar-tensor model of gravitational interaction with localizable field energy. The gravidynamics model shows the total mass (\({{M}_{{\text{Q}}}}\)) of a compact relativistic object filled with matter of quark-gluon plasma of the radius \(r\text{*} = G{{M}_{{\text{Q}}}}\)/c\(^{2} \approx 10\) km, consistent with the “m-gap”. It was conceptualized that the total measurable gravitational mass of such an extremely dense object consists of both matter and field, which is described by scalar-tensor components. This model is also useful for predicting the collapsars within “m-gap”.

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Funding

The work was performed as part of the government contract of the SAO RAS approved by the Ministry of Science and Higher Education of the Russian Federation. The authors are grateful to T.N. Sokolova for help in preparing the manuscript.

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  1. Institute for Physics ofMicrostructures, Russian Academy of Sciences, 603087, Nizhny Novgorod, Russia

    N. Kumar

  2. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia

    V. V. Sokolov

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Kumar, N., Sokolov, V.V. Mass Distribution and “Mass Gap” of Compact Stellar Remnants in Binary Systems. Astrophys. Bull. 77, 197–213 (2022). https://doi.org/10.1134/S1990341322020043

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