Stability of super-Chandrasekhar magnetic white dwarfs

Chamel, Nicolas; Fantina, Anthea; Davis, Philip J.

doi:10.1103/physrevd.88.081301

Cited by 56 publications

(88 citation statements)

References 39 publications

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“…The inner region of white dwarfs, in particular for B int 10 17 G, would have been neutronized if the drip density had not been changed with the field. Note that some authors have questioned the existence of such white dwarfs [14]. For example, the authors have argued that for the white dwarfs to be stable against neutronization, the magnetic field at the center should be less than few times 10 16 G for typical matter compositions.…”

Section: Discussionmentioning

confidence: 99%

Revised density of magnetized nuclear matter at the neutron drip line

Vishal¹,

Mukhopadhyay²

2014

Phys. Rev. C

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We study the onset of neutron drip in high density matter in the presence of magnetic field. It has been found that for systems having only protons and electrons, in the presence of magnetic field 10 15 G, the neutronization occurs at a density which is atleast an order of magnitude higher compared to that in a nonmagnetic system. In a system with heavier ions, the effect of magnetic field, however, starts arising at a much higher field, 10 17 G. These results may have important implications in high magnetic neutron stars and white dwarfs and, in general, nuclear astrophysics when the system is embedded with high magnetic field.

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Section: Discussionmentioning

confidence: 99%

Revised density of magnetized nuclear matter at the neutron drip line

Vishal¹,

Mukhopadhyay²

2014

Phys. Rev. C

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“…In a related context, some authors [17] have suggested that the onset of neutronization and pycnonuclear reactions may limit the stability of the concerned super-Chandrasekhar white dwarfs, due to a softening of the underlying EoS. We recall here that a similar softening is brought about when a constant ρ B is added to ρ, without changing the pressure, while solving for the structure of the white dwarf.…”

mentioning

confidence: 92%

“…However, this is equally valid for nonmagnetized Chandrasekhar's white dwarfs whose central ρ is ∼ 10 9 gm/cc as well. The authors [17] further show that for the white dwarfs to be stable against neutronization, B at the center should be less than few times 10 16 G for typical matter compositions. Note that, as mentioned before at the end of §5, for B cent 10 16 G the mass-radius relation already starts approaching the limiting mass, yielding super-Chandrasekhar white dwarfs with mass 2.44M ⊙ , in the Newtonian regime itself.…”

mentioning

confidence: 99%

Revisiting some physics issues related to the new mass limit for magnetized white dwarfs

Das

Mukhopadhyay

2014

Mod. Phys. Lett. A

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We clarify important physics issues related to the recently established new mass limit for magnetized white dwarfs which is significantly super-Chandrasekhar. The issues include, justification of high magnetic field and the corresponding formation of stable white dwarfs, contribution of the magnetic field to the total density and pressure, flux freezing, variation of magnetic field and related currents therein. We also attempt to address the observational connection of such highly magnetized white dwarfs.

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“…On the other hand, Hillebrandt, Sim & Röpke (2007) and Hachinger et al (2013) have argued that the explosion of a rotating super-M Ch WD will not necessarily produce the inferred nickel mass, or other characteristics, of such bright events, and they have suggested asymmetric explosions instead (see also Moll et al 2013). Chamel, Fantina & Davis (2013) have shown that another proposed means of supporting super-M Ch WDs, via ultra-strong quantizing magnetic fields, is impractical, due to electron-capture reactions that would make the WD unstable.…”

Section: Double Detonations and Rotating Super-chandrasekhar-mass Modelsmentioning

confidence: 99%

Observational Clues to the Progenitors of Type Ia Supernovae

Maoz

Mannucci

Nelemans

2014

Annu. Rev. Astron. Astrophys.

965

894

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Type-Ia supernovae (SNe Ia) are important distance indicators, element factories, cosmic-ray accelerators, kinetic-energy sources in galaxy evolution, and endpoints of stellar binary evolution. It has long been clear that a SN Ia must be the runaway thermonuclear explosion of a degenerate carbon-oxygen stellar core, most likely a white dwarf (WD). However, the specific progenitor systems of SNe Ia, and the processes that lead to their ignition, have not been identified. Two broad classes of progenitor binary systems have long been considered: single-degenerate (SD), in which a WD gains mass from a non-degenerate star; and doubledegenerate (DD), involving the merger of two WDs. New theoretical work has enriched these possibilities with some interesting updates and variants. We review the significant recent observational progress in addressing the progenitor problem. We consider clues that have emerged from the observed properties of the various proposed progenitor populations, from studies of their sites -pre-and post-explosion, from analysis of the explosions themselves, and from the measurement of event rates. The recent nearby and well-studied event, SN 2011fe, has been particularly revealing. The observational results are not yet conclusive, and sometimes prone to competing theoretical interpretations. Nevertheless, it appears that DD progenitors, long considered the underdog option, could be behind some, if not all, SNe Ia. We point to some directions that may lead to future progress.

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Stability of super-Chandrasekhar magnetic white dwarfs

Cited by 56 publications

References 39 publications

Revised density of magnetized nuclear matter at the neutron drip line

Revised density of magnetized nuclear matter at the neutron drip line

Revisiting some physics issues related to the new mass limit for magnetized white dwarfs

Observational Clues to the Progenitors of Type Ia Supernovae

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