Relevance of Dynamical Nuclear Processes in Quantum Complex Systems of Massive White Dwarfs

Malheiro, M.; Otoniel, Edson; Coelho, Jaziel G.

doi:10.1007/s13538-020-00840-0

Cited by 1 publication

(2 citation statements)

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“…We recently performed a stability analysis of the matter in the cores of WDs against pycnonuclear fusion reactions and electron capture reactions (see Otoniel et al 2019;Malheiro et al 2021, for details). In the current paper we investigate the stability of carbon WD matter to pycnonuclear fusion reactions using up-to-date theoretical models (see Gasques et al 2005;Golf et al 2009).…”

Section: Pycnonuclear Fusion Reactionsmentioning

confidence: 99%

“…In this paper we describe WD matter in terms of helium, carbon, oxygen, or a mixture of oxygen (64%) and neon (36%), taking not only the electron Fermi gas contribution into account, but also the contributions from electron-ion, electron-electron, and ion-ion interactions. Recently, we performed a stability analysis of the matter in the cores of WDs against pycnonuclear fusion reactions (see Otoniel et al 2019;Malheiro et al 2021). In the present paper, we determine theoretical bounds on the mass of CTCV J2056-3014 that follow from mass shedding caused by rotation at the Kepler frequency and pycnonuclear fusion reactions among carbon nuclei in the core of WD matter.…”

Section: Introductionmentioning

confidence: 99%

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Mass limits of the extremely fast-spinning white dwarf CTCV J2056–3014

Otoniel

Coelho

Nunes

et al. 2021

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CTCV J2056–3014 is a nearby cataclysmic variable with an orbital period of approximately 1.76 h at a distance of about 853 light-years from the Earth. Its recently reported X-ray properties suggest that J2056–3014 is an unusual accretion-powered intermediate polar that harbors a fast-spinning white dwarf (WD) with a spin period of 29.6 s. The low X-ray luminosity and the relatively modest accretion rate per unit area suggest that the shock is not occurring near the WD surface. It has been argued that, under these conditions, the maximum temperature of the shock cannot be directly used to determine the mass of the WD (which, under the abovementioned assumptions, would be around 0.46 M⊙). Here, we explore the stability of this rapidly rotating WD using a modern equation of state (EoS) that accounts for electron–ion, electron–electron, and ion–ion interactions. For this EoS, we determine the mass density thresholds for the onset of pycnonuclear fusion reactions and study the impact of microscopic stability and rapid rotation on the structure and stability of WDs, considering them with helium, carbon, oxygen, and neon. From this analysis, we obtain a minimum mass for CTCV J2056–3014 of 0.56 M⊙ and a maximum mass of around 1.38 M⊙. If the mass of CTCV J2056–3014 is close to the lower mass limit, its equatorial radius would be on the order of 104 km due to rapid rotation. Such a radius is significantly larger than that of a nonrotating WD of average mass (0.6 M⊙), which is on the order of 7 × 103 km. The effects on the minimum mass of J2056–3014 due to changes in the temperature and composition of the stellar matter were found to be negligibly small.

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