Workshop_2015

The International Workshop on
Quark Phase Transition in Compact Objects and Multimessenger Astronomy:
Neutrino Signals, Supernovae and Gamma-Ray Bursts

7-14 October 2015

On the observed mass distribution of compact stellar remnants in close binary systems and possible interpretations proposed for the time being

Sokolov V.V.

Abstract

      It turns out that accumulation of data during 40-years observational studies just emphasized a contrast between pulsars and black hole (BH) candidates in Galactic close binary stellar systems: (1) the mass spectrum of these degenerate stellar objects (or collapsars) shows an evident absence of objects with masses within the interval from 2M⊙ (with a first peak at about 1.4M⊙) to approximately 6M⊙, (2) and in close binary stellar systems with a low-massive (about 0.6M⊙) optical companion the most probable mass value (the peak in the mass distribution of BH candidates) turned out to be close to 6.7M⊙. This puzzle of discrete mass spectra of collapsars in close binary systems demands some solution and explanation in stellar evolution scenarios in connection with the core-collapse supernovae explosion mechanism and in context of a relation between supernovae and gamma-ray bursts. The collapsar strong field - an analogue of BH in General Relativity - is investigated in a totally non-metric, dynamical model of gravitational interaction theory, in which extremely compact objects of the masses MQ ≈ 6.7M⊙ with a quark-gluon plasma bag of radius r* = GMQ/c2 ≈ 10 km exist.

Reference:
Sokolov V.V., "On the observed mass distribution of compact stellar remnants in close binary systems and possible interpretations proposed for the time being", in "Proceedings of the International Workshop on Quark Phase Transition in Compact Objects and Multimessenger Astronomy: Neutrino Signals, Supernovae and Gamma-Ray Bursts", Russia, Nizhnij Arkhyz (SAO RAS), Terskol (BNO INR RAS), October, 7 - 14, 2015, Publishing house "Sneg", Pyatigorsk, 2016, ISBN 978-5-903129-85-0, pp. 121-132.
DOI: 10.26119/SAO.2020.1.51263
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