Consequence of total lepton number violation in strongly magnetized iron white dwarfs

Belyaev, V.B.; Ricci, P.; Šimkovic, F.; Adam, J.; Tater, Miloš; Truhlík, E.

doi:10.1016/j.nuclphysa.2015.02.002

Cited by 19 publications

(15 citation statements)

References 119 publications

(268 reference statements)

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“…In this work we investigate the time evolution of massive, uniformly rotating, highly magnetized white dwarfs (WDs) when they lose angular momentum owing to magnetic dipole braking. We have different important reasons to perform such an investigation: 1) there is incontestable observational data on the existence of massive (M ∼ 1 M ) WDs with magnetic fields all the way to 10 9 G (see (Kepler et al 2015), and references therein); 2) WDs can rotate with periods as short as P ≈ 0.5 s (Boshkayev et al 2013b); 3) they can be formed in double WD mergers (García-Berro et al 2012;Rueda et al 2013;Kilic et al 2018); 4) they have been invoked to explain type Ia supernovae within the double degenerate scenario (Webbink 1984;Iben & Tutukov 1984); 5) they constitute a viable model to explain soft gamma-repeaters and anomalous Xray pulsars (Malheiro et al 2012;Boshkayev et al 2013a;Rueda et al 2013;Boshkayev et al 2015a;Belyaev et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Time evolution of rotating and magnetized white dwarf stars

Becerra

Boshkayev

Rueda

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of isolated, zero and finite temperature, massive, uniformly rotating and highly magnetized white dwarf stars under angular momentum loss driven by magnetic dipole braking. We consider the structure and thermal evolution of white dwarf isothermal cores taking also into account the nuclear burning and neutrino emission processes. We estimate the white dwarf lifetime before it reaches the condition either for a type Ia supernova explosion or for the gravitational collapse to a neutron star. We study white dwarfs with surface magnetic fields from 10 6 to 10 9 G and masses from 1.39 to 1.46 M and analyze the behavior of the white dwarf parameters such as moment of inertia, angular momentum, central temperature and magnetic field intensity as a function of lifetime. The magnetic field is involved only to slow down white dwarfs, without affecting their equation of state and structure. In addition, we compute the characteristic time of nuclear reactions and dynamical time scale. The astrophysical consequences of the results are discussed.

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Section: Introductionmentioning

confidence: 99%

Time evolution of rotating and magnetized white dwarf stars

Becerra

Boshkayev

Rueda

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Such Super-Chandrasekhar mass white dwarfs could be possible progenitors of over-luminous type-Ia supernovae (Howell et al 2006;Hicken et al 2007;Yamanaka et al 2009;Scalzo et al 2010;Tanaka et al 2010;Silverman et al 2011;Taubenberger et al 2011). Several publications in the recent literature have addressed different aspects of this issue: for example, the effects of magnetic field on the equation of state (Das & Mukhopadhyay 2012;Manreza Paret et al 2015;Zou & Meng 2015;Mukhopadhyay et al 2015), Lorentz force and instability (Nityananda & Konar 2014;Coelho et al 2014), possibility of electron capture (Chamel et al 2013(Chamel et al , 2014Vishal & Mukhopadhyay 2014) and total lepton number violation (Belyaev et al 2015). In an earlier work (hereafter P1, Bera & Bhattacharya (2014)) we have presented the massradius relation of strongly magnetized white dwarfs with self consistent inclusion of Lorentz force.…”

Section: Introductionmentioning

confidence: 99%

Mass–radius relation of strongly magnetized white dwarfs: dependence on field geometry, GR effects and electrostatic corrections to the EOS

Bera

Bhattacharya

2016

Mon. Not. R. Astron. Soc.

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Recent literature has seen an ongoing discussion on the limiting mass of strongly magnetized white dwarfs, since such objects may prove to be a source of over-luminous type-Ia supernovae. In an earlier paper, we have presented the mass-radius relation of white dwarfs with a strong poloidal magnetic field in Newtonian gravity. The inclusion of effects such as general relativistic gravity and many-body corrections to the equation of state can alter the mass-radius relation and the maximum mass. In this work we estimate the extent to which these effects may modify the earlier results. We find that the general relativistic effects tend to reduce the maximum mass by about 2% and many-body corrections by another additional ∼2%, for an assumed carbon composition. We also explore field geometries that are purely toroidal or a mixture of poloidal and toroidal and find that the limiting mass of such equilibrium configurations can be substantially higher than in the case of a purely poloidal field.

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“…Sub-Chandrasekhar limiting-mass WDs were believed to be formed by merging two sub-Chandrasekhar mass WDs (double-degenerate scenario), leading to another sub-Chandrasekhar mass WD, exploding due to accretion of a helium layer (Hillebrandt & Niemeyer 2000;Pakmor et al 2010). On the other hand, the super-Chandrasekhar WDs were often explained by incorporating different physics, such as a double-degenerate scenario (Hicken et al 2007), presence of magnetic fields (Das & Mukhopadhyay 2013, presence of a differential rotation (Hachisu et al 2012), presence of charge in the WDs (Liu et al 2014), ungravity effect (Bertolami & Mariji 2016), lepton number violation in magnetized WD (Belyaev et al 2015), generalized Heisenberg uncertainty principle (Ong 2018), and many more. However, none of these theories can self-consistently explain both of the peculiar classes of WDs.…”

Section: Introductionmentioning

confidence: 99%

Gravitational Wave in f(R) Gravity: Possible Signature of Sub- and Super-Chandrasekhar Limiting-mass White Dwarfs

Kalita

Mukhopadhyay

2021

ApJ

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After the prediction of many sub-and super-Chandrasekhar (at least a dozen for the latter) limiting-mass white dwarfs (WDs), hence apparently a peculiar class of WDs, from the observations of luminosity of Type Ia supernovae, researchers have proposed various models to explain these two classes of WD separately. We earlier showed that these two peculiar classes of WD, along with the regular WD, can be explained by a single form of the f (R) gravity, whose effect is significant only in the high-density regime, and it almost vanishes in the low-density regime. However, since there is no direct detection of such a WD, it is difficult to single out one specific theory from the zoo of modified theories of gravity. We discuss the possibility of direct detection of such a WD in gravitational wave (GW) astronomy. It is well known that in f (R) gravity more than two polarization modes are present. We estimate the amplitudes of all the relevant modes for the peculiar and the regular WD. We further discuss the possibility of their detections through future-based GW detectors, such as LISA, ALIA, DECIGO, BBO, or the Einstein Telescope, and thereby put constraints on or rule out various modified theories of gravity. This exploration links the theory with possible observations through GW in f (R) gravity.

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Consequence of total lepton number violation in strongly magnetized iron white dwarfs

Abstract: The influence of a neutrinoless electron to positron conversion on a cooling of strongly magnetized iron white dwarfs is studied. It is shown that they can be good candidates for soft gamma-ray repeaters and anomalous X-ray pulsars.

Cited by 19 publications

References 119 publications

Time evolution of rotating and magnetized white dwarf stars

Time evolution of rotating and magnetized white dwarf stars

Mass–radius relation of strongly magnetized white dwarfs: dependence on field geometry, GR effects and electrostatic corrections to the EOS

Gravitational Wave in f(R) Gravity: Possible Signature of Sub- and Super-Chandrasekhar Limiting-mass White Dwarfs

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