Relativistic formulation of the Hall-Vinen-Bekarevich-Khalatnikov superfluid hydrodynamics

Gusakov, M. E.

doi:10.1103/physrevd.93.064033

Cited by 26 publications

(78 citation statements)

References 50 publications

(146 reference statements)

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“…where n n,th ≡ n n −µ n Y nn is the number density of (normal) neutron thermal excitations and Y nn is the nn component of the relativistic entrainment matrix [42][43][44][45][46] (all other components of this matrix vanish when protons are normal).…”

Section: Superfluidity/superconductivitymentioning

confidence: 99%

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Evolution of the magnetic field in neutron stars

2017

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Section: Superfluidity/superconductivitymentioning

confidence: 99%

“…(55) describes the motion of the superfluid neutron component (see, e.g., Refs. [42,45,46]). As in Sec.…”

Section: Superfluidity/superconductivitymentioning

confidence: 99%

Evolution of the magnetic field in neutron stars

2017

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“…In this section we describe oscillations of superfluid NS using the Newtonian limit of relativistic hydrodynamics, formulated by Gusakov (2016); Gusakov & Dommes (2016). We consider a slowly rotating (with the spin frequency Ω) NS with the core composed of neutrons, protons and electrons.…”

Section: Equations Governing Oscillations Of a Rotating Superfluid Nsmentioning

confidence: 99%

Temperature-dependent oscillation modes in rotating superfluid neutron stars

Dommes

Kantor

Gusakov

2018

Monthly Notices of the Royal Astronomical Society

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We calculate the spectrum of inertial oscillation modes in a slowly rotating superfluid neutron star, including, for the first time, both the effects of finite temperatures and entrainment between superfluid neutrons and protons. We work in the Newtonian limit and assume minimal core composition (neutrons, protons and electrons). We also developed an approximate method that allows one to calculate the superfluid r-mode analytically. Finally, we derive and analyze dispersion relations for inertial modes in the superfluid NS matter in the short wavelength limit.

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“…In our analysis we shall use the Newtonian limit of the relativistic hydrodynamics, formulated in Gusakov (2016); and describing rotating superfluid mixture at a finite temperature. Below we formulate the main equations of this hydrodynamics.…”

Section: General Equations Of Superfluid Hydrodynamicsmentioning

confidence: 99%

“…The general relativistic expression for the oscillation energy dissipation rate due to mutual friction (per unit volume), ǫMF, can be deduced from (see also Kantor & Gusakov 2012;Gusakov 2016). In the Newtonian limit, we are interested in here, the corresponding expression can be obtained by making use of the equation (90) from , as well as the formulas (6) and (7) and the definition of z z z.…”

Section: Dissipative Damping Of R-modesmentioning

confidence: 99%

Temperature-dependent r modes in superfluid neutron stars stratified by muons

Kantor¹,

Gusakov²

2017

Monthly Notices of the Royal Astronomical Society

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We calculate the finite-temperature r-mode spectrum of a slowly rotating superfluid Newtonian neutron star neglecting the entrainment between neutron and proton liquid components (i.e., neglecting the off-diagonal element of the entrainment matrix). We show that for 'minimal' NS core composition (neutrons, protons, and electrons) only two m = 2 r-modes exist -normal mode, which is similar to ordinary r-mode in a nonsuperfluid star, and a superfluid temperature-dependent mode. Accounting for muons in the core dramatically modifies the oscillation spectrum, resulting in an infinite set of superfluid r-modes, whose frequencies vary with temperature. We demonstrate that the normal r-mode can exhibit avoided crossings with superfluid modes at certain 'resonance' temperatures, where it dissipates strongly, which leads to substantial suppression of the r-mode instability near these temperatures. The corresponding instability windows are calculated and discussed. 1 Following Gusakov et al. (2014a), by the normal r-modes of a superfluid NS we mean the modes which, at a given temperature, have properties similar to ordinary r-modes in the non-superfluid NSs. They correspond to co-motion of superfluid and normal liquid components, and their eigenfrequencies do not depend on temperature. Normal r-modes are most unstable. By superfluid inertial modes we understand inertial modes which show superfluid-like behaviour at a given temperature. The oscillations of such modes are mostly counter-moving, baryon current is almost zero, their eigenfrequencies depend on temperature. These modes have no analogue in nonsuperfluid NSs. Note that, with temperature variation, a given mode can switch from a 'superfluid' regime to 'normal' regime and vice versa, experiencing avoided-crossings with neighbouring modes.

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Relativistic formulation of the Hall-Vinen-Bekarevich-Khalatnikov superfluid hydrodynamics

Cited by 26 publications

References 50 publications

Evolution of the magnetic field in neutron stars

Evolution of the magnetic field in neutron stars

Temperature-dependent oscillation modes in rotating superfluid neutron stars

Temperature-dependent r modes in superfluid neutron stars stratified by muons

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