Time evolution of rotating and magnetized white dwarf stars

Becerra, L.; Boshkayev, Kuantay; Rueda, J. A.; Ruffini, Remo

doi:10.1093/mnras/stz1394

Cited by 8 publications

(7 citation statements)

References 53 publications

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“…Simulations of mergers of WDs leading to magnetic super-Chandrasekhar WDs have been performed [65] leading to a maximum mass of 1.45 M . For the case of isolated sources, it would be 1.46 M [10]. This is in accordance with new observations such as the one in Ref.…”

Section: Massive White Dwarfs On the Grounds Of Modified Gravitysupporting

confidence: 92%

“…In this context, plenty of works have been done to model these very massive white dwarfs (MWD). The properties of MWDs have been studied in different contexts: rotation [7][8][9][10]; high electric and magnetic fields [11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26]; temperature [27,28] and modified gravity [29][30][31][32][33][34][35][36][37][38][39][40]. It has been shown that general relativistic effects are essential for massive white dwarfs and cannot a e-mail: r.vieira@uniandes.edu.co b e-mail: araujogc@ita.br c e-mail: nkelkar@uniandes.edu.co d e-mail: mnowakos@uniandes.edu.co (corresponding author) be disregarded [41][42][43][44][45].…”

Section: Introductionmentioning

confidence: 99%

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Massive white dwarfs in $$f(\mathtt {R,L_m})$$ gravity

et al. 2022

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In this work, we investigate the equilibrium configurations of massive white dwarfs (MWD) in the context of modified gravity, namely $$f(\mathtt {R,L_m})$$ f ( R , L m ) gravity, where $$\mathtt {R}$$ R stands for the Ricci scalar and $$\mathtt {L_m}$$ L m is the Lagrangian matter density. We focused on the specific case $$f(\mathtt {R,L_m})= \mathtt {R}/2 + \mathtt {L_m}+ \sigma \mathtt {R}\mathtt {L_m}$$ f ( R , L m ) = R / 2 + L m + σ R L m , i.e., we have considered a non-minimal coupling between the gravity field and the matter field, with $$\sigma $$ σ being the coupling constant. For the first time, the theory is applied to white dwarfs, in particular to study massive white dwarfs, which is a topic of great interest in the last years. The equilibrium configurations predict maximum masses which are above the Chandrasekhar mass limit. The most important effect of the theory is to increase significantly the mass for stars with radius < 2000 km. We found that the theory can accommodate the super-Chandrasekhar white dwarfs for different star compositions. Apart from this, the theory recovers the General Relativity results for stars with radii larger than 3000 km, independent of the value of $$\sigma $$ σ .

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Section: Massive White Dwarfs On the Grounds Of Modified Gravitysupporting

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Massive white dwarfs in $$f(\mathtt {R,L_m})$$ gravity

et al. 2022

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“…There are also a plethora of observational data for carbon and other WDs [23,24]. The time and thermal evolution of carbon WDs has been theoretically investigated involving the nuclear burning and neutrino emission processes [25]. The observational support of the existence of iron-rich cores of WDs was given in Ref.…”

Section: Problem Setup and Methodologymentioning

confidence: 99%

Static and rotating white dwarf stars at finite temperatures

Boshkayev¹,

Luongo²,

Muccino³

et al. 2021

ijmph

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Static and rotating, cold and hot white dwarf stars are investigated both in Newtonian gravity and general theory of relativity, employing the well-established Chandrasekhar equation of state. The Hartle formalism is involved to construct and study uniformly rotating configurations of white dwarfs. The mass-radius, mass-central density, radius-central density and other basic relations of stable white dwarfs, consisting of pure helium and iron, are constructed for different temperatures at mass shedding limit. Stability of white dwarfs is analyzed with respect to the inverse beta decay process, pycnonuclear reactions and instabilities of general relativity. It is found that for a fixed mass hot white dwarfs consisting of pure iron are smaller in size, correspondingly denser with respect to the ones composed of light elements. In addition, it is shown that near the Chandrasekhar mass limit the mass of hot rotating white dwarfs is slightly less than for cold ones, though for low mass rotating white dwarfs and static ones in all mass range the situation is opposite.

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“…It is well know that unlike magnetic field or anisotropic pressure, rotation is the main contributor to the deformation of compact objects such as WDs and NSs [69][70][71]. Here by exploiting the HT formalism [37,38,72] the rotating equilibrium configurations of WDs [73,74] and NSs [69,75,76] are constructed and the mass quadrupole moment as a function of central density for maximally rotating stars (see Fig.…”

Section: Rotating White Dwarfs and Neutron Starsmentioning

confidence: 99%

Neutrino oscillation in the q-metric

2020

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We investigate neutrino oscillation in the field of an axially symmetric space-time, employing the so-called q-metric, in the context of general relativity. Following the standard approach, we compute the phase shift invoking the weak and strong field limits and small deformation. To do so, we consider neutron stars, white dwarfs and supernovae as strong gravitational regimes whereas the solar system as weak field regime. We argue that the inclusion of the quadrupole parameter leads to the modification of the well-known results coming from the spherical solution due to the Schwarschild space-time. Hence, we show that in the solar system regime, considering the Earth and Sun, there is a weak probability to detect deviations from the flat case, differently from the case of neutron stars and white dwarfs in which this probability is larger. Thus, we heuristically discuss some implications on constraining the free parameters of the phase shift by means of astrophysical neutrinos. A few consequences in cosmology and possible applications for future space experiments are also discussed throughout the text.

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Time evolution of rotating and magnetized white dwarf stars

Cited by 8 publications

References 53 publications

Massive white dwarfs in $$f(\mathtt {R,L_m})$$ gravity

Massive white dwarfs in $$f(\mathtt {R,L_m})$$ gravity

Static and rotating white dwarf stars at finite temperatures

Neutrino oscillation in the q-metric

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