Relativistic Feynman-Metropolis-Teller treatment at finite temperatures

Carvalho, Sheyse Martins de; Rotondo, Michael F.; Rueda, J. A.; Ruffini, Remo

doi:10.1103/physrevc.89.015801

Cited by 35 publications

(40 citation statements)

References 21 publications

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“…For α = 0, our predictions for the maximum mass of WDs are in good agreement with the classical results of Chandrasekhar (see e.g., Carvalho et al ) using the conventional formulation of GR. Our calculations for other values of the α parameter predict values of maximum masses of WDs much larger than the results observed so far.…”

Section: Results and Conclusionsupporting

confidence: 88%

Equilibrium configurations of white dwarfs in the pseudo‐complex general relativity

et al. 2017

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Observations of type Ia supernovae (SNe Ia) admit white dwarfs (WDs) with masses as high as 2.3−2.6M⊙, surpassing in this way the mass limit of WDs established by Chandrasekhar (1.44M⊙). Within the scope of pseudo‐complex general relativity (pc‐GR), we investigate a possible mechanism for such a hypothesis, using a very simple model for the WD matter, which consists in our approach of ionized hydrogen and helium nuclei (nucleons) and electrons. In pc‐GR, the field equations have an extra term compared to the field equations of Einstein's general relativity. This additional term is associated with the nature of spacetime, of repulsive character, which is believed to halt the gravitational attractive collapse of matter distributions in the evolution process of compact stars. This additional term arises from microscale phenomena due to vacuum fluctuations, which simulate the presence of dark energy in the Universe. In a more conventional theoretical description of a WD, the electron degeneracy pressure ultimately stabilizes the star against collapse. In this paper, we explore the presence of this additional term of pc‐GR and study the role of dark energy in the structure of WDs, constituted by nucleons and electrons and held together by the presence of the gravitational interaction, and superimposed on a repulsive background of dark energy. The corresponding versions of the Tolman–Oppenheimer–Volkoff (TOV) equations in the pc‐GR formalism are solved, and the mass–radius relations as well as the maximum mass of the WD star are determined for different parameter configurations.

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Section: Results and Conclusionsupporting

confidence: 88%

Equilibrium configurations of white dwarfs in the pseudo‐complex general relativity

et al. 2017

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“…For mass densities below about 10 4 g=cm 3 , an atmosphere of partially ionized atoms and electrons forms the outer part of a NS with an EoS given by Feynman, Metropolis, and Teller (1949), Rotondo et al (2011), andde Carvalho et al (2014). At higher densities, the spatial region that is made up of inhomogeneous nucleonic matter and electrons not bound to nuclei in β equilibrium is called the crust.…”

Section: Neutron Star Crust Eoss and Unified Neutron Star Eossmentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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“…In view of the latest observational data on WDs, [15][16][17] it would be interesting to explore WDs, taking into account the Coulomb and Thomas-Fermi corrections at finite temperatures in the EoS as in Ref. 6, including the effects of rotation in the structure equations. That will be the issue of future studies.…”

Section: Resultsmentioning

confidence: 99%