Dark matter admixed neutron stars

Kain, Ben

doi:10.1103/physrevd.103.043009

Cited by 51 publications

(56 citation statements)

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“…log( P om (0) [MeV/fm 3 ] ) (33) is much faster, but it cannot compute radial oscillation frequencies. It was confirmed in [44] that these two methods give the same result for critical curves, as expected.…”

Section: A Stabilitysupporting

confidence: 78%

“…Since both ordinary and dark matter have the same equation of state, Fig. 3 is symmetric in the two fluids, but this does not hold in general [44]. Static solutions enclosed by the critical curve (i.e.…”

Section: A Stabilitymentioning

confidence: 96%

“…(32). Interestingly, in the upper right corner, there exist linearly stable static solutions that would not be deemed so by a naive single-fluid analysis, which appears to be a general phenomena [44].…”

Section: A Stabilitymentioning

confidence: 97%

“…A linear stability analysis of dark matter admixed neutron stars, as analyzed using the two methods described above, was given in [44]. Here, we extend this analysis with a study of nonlinear stability by dynamically evolving static solutions.…”

Section: A Stabilitymentioning

confidence: 97%

“…These points give the critical curve. (For a derivation of this result, as well as the equations for computing N om and N dm from an equation of state, see [44]. )…”

Section: A Stabilitymentioning

confidence: 99%

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Dynamical evolution of dark matter admixed neutron stars

Gleason,

Brown,

Kain

2022

Preprint

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We dynamically evolve for the first time dark matter admixed neutron stars with fermionic dark matter. These systems are mixtures of the ordinary nuclear matter of a neutron star and dark matter. To perform our dynamical evolutions, we derive the equations of motion, in conservation form, for spherically symmetric systems with an arbitrary number of perfect fluids. Using finite volume and high-resolution shock-capturing methods, we dynamically evolve the two-fluid case, with the first fluid modeling ordinary matter and the second fluid modeling dark matter. We use our dynamical solutions to study nonlinear stability, radial oscillation frequencies, and a dynamical formation process.

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Section: A Stabilitysupporting

confidence: 78%

Section: A Stabilitymentioning

confidence: 96%

Section: A Stabilitymentioning

confidence: 97%

Section: A Stabilitymentioning

confidence: 97%

“…These points give the critical curve. (For a derivation of this result, as well as the equations for computing N om and N dm from an equation of state, see [44]. )…”

Section: A Stabilitymentioning

confidence: 99%

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