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Noncommutative dispersion relation and mass-radius relation of white dwarfs

Research in Astronomy and Astrophysics 2018年第12期18卷 75-88页

作者： Arun Mathew malay k.nandy Department of Physics Indian Institute of Technology Guwahati

The equation of state of the electron degenerate gas in a white dwarf is usually treated by employing the ideal dispersion ***, the effect of quantum gravity is expected to be inevitably present and when this effect is considered through a non-commutative formulation, the dispersion relation undergoes a substantial *** this paper, we take such a modified dispersion relation and find the corresponding equation of state for the degenerate electron gas in white *** we solve the equation of hydrostatic equilibrium and find that this leads to the possibility of the existence of excessively high values of masses exceeding the Chandrasekhar limit, although the quantum gravity effect is taken to be very *** is only when we impose the additional effect of neutronization that we obtain white dwarfs with masses close to the Chandrasekhar limit with nonzero radii at the neutronization *** demonstrate these results by giving numerical estimates for the masses and radii of helium, carbon and oxygen white dwarfs.

关键词： gravitation equation of state stars:white dwarfs

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General relativistic calculations for white dwarfs

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Research in Astronomy and Astrophysics 2017年第6期17卷 107-116页

作者： Arun Mathew malay k. nandy Department of Physics Indian Institute of Technology Guwahati Guwahati 781 039 India

The mass-radius relations for white dwarfs are investigated by solving the Newtonian as well as Tolman-Oppenheimer-Volkoff （TOV） equations for hydrostatic equilibrium assuming the electron gas to be non-interacting. We find that the Newtonian limiting mass of 1.4562 M is modified to 1.4166 M in the general relativistic case for 4He （and 12 6C） white dwarfs. Using the same general relativistic treatment, the critical mass for 56 26Fe white dwarfs is obtained as 1.2230 M. In addition, departure from the ideal degenerate equation of state （EoS） is accounted for by considering Salpeter＇s EoS along with the TOV equation, yielding slightly lower values for the critical masses, namely 1.4081 M for 4He, 1.3916M for 12C and 1.1565M for 56 26Fe white dwarfs. We also compare the critical densities for gravitational instability with the neutronization threshold densities to find that 4 2He and 12 6C white dwarfs are stable against neutronization with the critical values of 1.4081 M and 1.3916 M, respectively. However, the critical masses for 16 8O, 20 10Ne, 24 12Mg, 28 14Si,32 16S and 56 26Fewhite dwarfs are 26Fe white lower due to neutronization. Corresponding to their central densities for neutronization thresholds, we obtain their maximum stable masses due to neutronization by solving the TOV equation coupled with the Salpeter EoS.

关键词： equation of state - hydrodynamics-instabilities - relativistic processes - stars whitedwarfs

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