On the energy budget of the transition of a neutron star into the third family branch

Abstract

Transition of a compact star into the third family for an equation of state (EoS) featuring mass twins is considered. The energy released at a baryon number conserving transition for static compact stars configurations is computed for two sets of models for comparison. The EoS of choice is the density dependent functional DD2 EoS with excluded model correction for hadronic matter which suffers a phase transition into deconfined quark matter described by a constant speed of sound approach. The two sets of EoS models feature different compact star mass onsets that maximize the energy and radius difference at the transition while simultaneously fulfilling state-of-the-art constraints from multi-messenger astronomy and empirical nuclear data. It is found that the maximal energy budget at the transitions falls in the range of $10^{49}$ - $10^{52}$ ergs.

5 pages, 6 figures. Typos corrected, Figures 3 and 4 updated

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Cited by in corpus (8)

• Speed of Sound in Hybrid Stars and the Role of Bag Pressure in the Emergence of Special Points on M-R Variation of Hybrid Stars
• Probing hadron-quark phase transition in twin stars using $f$-modes
• A Detailed Analysis of the Special Points on $M-R$ Solutions of Hybrid (Twin) Stars
• Studying VLOCV twin compact stars with binary mergers
• Asymptotically conformal CFL quark matter within a nonlocal chiral quark model
• Formation of twin compact stars in low-mass X-ray binaries: Implications on eccentric and isolated millisecond pulsar populations
• Properties of the Object HESS J1731-347 as a Twin Compact Star
• Studying the variation of fundamental constants at the Cosmic Ray Extremely Distributed Observatory